COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     NUMBER 598

                              Konkoly Observatory
                              Budapest
                              1971 December 6




      FURTHER REMARKS CONCERNING VARIABLE 14 IN M5


      In a recent note in this Bulletin (Osborn, 1971)
the results of a surface gravity and effective temperature
determination were presented for the M5 star Arp II-51
(Arp, 1955) which, based on Bailey's (1917) chart of the
variables in M5, had been identified as Variable 14 of the
cluster. It was noted that from Arp's (1962) UBV colors of
the star its position in the cluster H-R diagram was 
inconsistent with that of an RR Lyrae type variable as the
period indicates Variable 14 is. However, Coutts (1971) and
Kukarkin (1971) have pointed out that Variable 14 is marked
incorrectly on Bailey's chart, and rather that II-51, the
star marked, the variable is the star 20 seconds of arc to
the east. Because of this confusion the following additional
information concerning my observations is presented.
      Star II-51 was observed as part of a program of
measuring the surface gravities, effective temperatures,
and metal abundances of a number of late-type globular
cluster stars by use of intermediate-band photoelectric
photometry. The star was observed with the David Dunlap 
Observatory (DDO) intermediate-band system on four nights in
1969 at the Kitt Peak National Observatory. The reduction
of these observations gave consistent values for the DDO
colors but yielded magnitudes of (DDO system) 15.42, 15.44,
15.54 and 15.56 for the four nights. Both this range of
0.14 magnitudes and the standard deviation of the measures
were the largest of any of the stars on the observing
program, including several objects over a magnitude fainter
and hence considerably more difficult. These facts suggested 
that II-51 might be a variable and thus its position in
the cluster was compared with those of the known variables
using Bailey's chart, which led to the mis-identification.
      It is noted that the observing notes and the reductions 
have been re-examined and confirm both the derived
magnitudes and that it was indeed II-51 that was observed
and not the variable. Whether or not II-51 is in fact also
a variable as indicated by the DDO observations should be
investigated.



                          WAYNE OSBORN
                     Proyecto de Astrofisica
                          Apartado 264
                       Merida, Edo. Merida
                          Venezuela



Arp, H.C. (1955) Astron. J. 60, 317. [BIBCODE 1955AJ.....60..317A ]
Arp, H. (1962) Astrophys. J. 135, 311. [BIBCODE 1962ApJ...135..311A ]
Bailey, S.I. (1917) Harvard Ann, 78, 99. [BIBCODE 1917AnHar..78...99B ]
Coutts, C. (1971) I.A.U. Inf. Bull. on Variable Stars,
      No 572.
Kukarkin, B.V. (1971) Astronomicheskii Tsirk., no. 646, [BIBCODE 1971ATsir.646....2K ]
Osborn, W. (1971) I.A.U. Inf.Bull. on Variable Stars,
      no. 563. [BIBCODE 1971IBVS..563....1O ]



               [DATAFILE 1]