COMMISSION 27 OF THE I. A. U.
           INFORMATION BULLETIN ON VARIABLE STARS
                        Number 935

                                      Konkoly Observatory
                                      Budapest
                                      1974 October 22


        PHOTOMETRY OF POSSIBLE ULTRASHORT PERIOD
            CEPHEIDS IN THE DISK POPULATIONS

   During the course of other programs with the 40-inch reflector
several bright candidates for ultrashort period cepheids have been
monitored, mainly during bright moonlight. The results for several
new variables have been published from time to time and the present
note contains the remainder observed thus far. Four new variables
are listed in Table 1 and the light curves are shown in the figures.
A dozen, probably constant stars are listed in Table 2 together with
the length of time (continuous) that the star was monitored, the 
comparison star used, the mean magnitude difference and the rms 
deviation from that mean.
   The columns of Table 1 contain the following information:
          I. HR/HD (name)
         II. V_E/B-V/U-B based on single observations with
             the 40-inch reflector.
        III. [m_1]/[c_1]/beta derived from photometry with
             the 40- and 16-inch reflectors.
         IV. Delta[m_1]/Delta[c_1]/M_V (Eggen 1971).
          V. mu_{alpha}/mu_{delta}/rho. The proper motions (0".001) are
             on the FK system with precessional corrections
             and rho is in km/sec.
         VI. U/V/W. Space motion vectors (km/sec).



Mount Stromlo and Siding Spring
Observatory                                O.J. EGGEN




References:

Eggen, O.J. 1967, The Magnetic and Related Stars (Ed.R.Cameron).
Eggen, O.J. 1969, Ap.J. 155, 701. [BIBCODE 1969ApJ...155..701E ]
Eggen, O.J. 1971, Pub. A.S.P., 83. 741. [BIBCODE 1971PASP...83..741E ]


                  Table   1
                NEW VARIABLES

   I        II      III      IV     V     VI
  1505     6.83     280     - 64   +36    +25
55 Eri    +0.38     697     +107   -29    -37
          +0.18    2.727   (+1.6)  +40.0  -13

  3350     5.10     218     +  4   -68    +17
 71935    +0.26     894     +205   +22    -22
          +0.14    2.766    +1.2   +24.7  -16

  4746     6.23     226     -  7   -92    +50
108506    +0.445    703     +286   -11    -29
          +0.075   2.673    +0.6   -12:   -19

  8102     6.48     202     + 20   +38    +40
201707    +0.31     875     +190   + 3    -16.5
          +0.15    2.765    +1.2   -39.2  +10


1505 ADS 3409, 10". The observations were made under excellent
     seeing conditions and the secondary component, G8 III, was
     used as a comparison star. More observations are needed
     but the star is almost certainly variable. The adopted
     luminosity is from a previous discussion (Eggen 1969) where
     the system was found to have the same space motion as the
     variable rho Puppis (HR3185).

3350 The period appears to be near 0d.07.

4746 The period may be near 0d.05. Previously (Eggen 1967)
     suspected to be a member of the Hyades Group (which it is not)
     and a short period variable. The radial velocity is variable.

8102 Additional observations are needed to confirm the variation.
     Probably a member of the Hyades group despite the relatively
     large value of Delta[m_1].


                  Table 2
          PROBABLY CONSTANT STARS

   HR/HD         T     C_p(*)   Delta{V}  RMS
                HRS

       550      2.0      593    0.100    0.002
       981      3.0     1025    0.050    0.002
HD   22413      1.5    22582    0.088    0.003
HD   43760      3.0    43393    0.015    0.003
      2661(*)   3.0     2674    0.534    0.005
      3140      3.0     3154    0.668    0.002
      4042      1.5     4068    0.977    0.001
      5348      3.0     5337    0.029    0.002
      6366      4.5     6389    0.055    0.002
      7101      4.5     7143    0.108    0.002
    133604(*)   3.5   HR5614    0.562    0.008
    137949      2.5   HR5750    0.870    0.003

(*) 2661 Var ?
  133604 Var ?


                         [FIGURE 1]
                         [FIGURE 2]
                         [FIGURE 3]
                         [FIGURE 4]