COMMISSION 27 OF THE I.A.U.
             INFORMATION BULLETIN ON VARIABLE STARS
                           NUMBER 98

                                       Konkoly Observatory
                                       Budapest
                                       5 June 1965


                           V SAGITTAE

  In a recent paper on V Sge (1) G. H. Herbig, G. W. Preston, J. Smak
and B. Paczynski have found that this star is an eclipsing variable,
I have re-examined the photographic observations of V Sge made 
between JD 2435627 and 2436461 (2). The discussion of these observations 
have confirmed Herbig's conclusions, namely:

1.- The depth of the primary minimum changes with the mean brightness 
of V Sge. It reaches 1m.3 when the variable is near its minimum.

2.- Sudden and rapid fluctuations of light occur in some phases of
the light curve.

3.- The scattering of photographic magnitudes outside eclipse blot
out the visibility of secondary minimum. The scattering is produced
by superposition of observations made on different nights.

4.- Herbig's elements have been slightly changed as follows:

         min hel = 2437889.9154 + 0d.514202 E

The observed minima are listed below:

   min hel                     min hel
JD 243....    E       O - C     JD 243....   E      O - C

5662.435    4332     +0d.043    5802.208   4060    -0d.047
 663.438    4330     +  .017    6079.416   3521    +  .006
 696.360    4266     +  .030     096.351   3488    -  .028
 697.374    4264     +  .016     371.417   2953    -  .060
 699.438    4260     +  .023     404.407   2889    +  .021
 716.373    4227     -  .010     424.435   2850    -  .005
 717.441    4225     +  .028     426.470   2846    -  .026
 782.213    4099     +  .012     461.422   2778    -  .040


1 Ap.J. Vol 141, no. 2, 617. [BIBCODE 1965ApJ...141..617H ]
2 Pubb. no. 119 Oss. Astronomico di Padova 1960

                                        G. ROMANO
                                   Padua Observatory
                                         Italy