In Table 1 (click here) we list some basic information for these variables
indentified in fields 5139A-F which were not discussed in Papers I
or II. The OGLEGC ID numbers assigned to variables are
continuation of the sequence from Papers I and II.
Some fraction of variables was observed in more than one field.
For such stars multiple entries are given in Table 1 (click here). Hence,
Table 1 (click here) lists in fact light curves which were obtained for
variables OGLEGC71-211. The field in which a given variable was observed is
listed in Cols. 2 and 10. The rectangular coordinates (X, Y)
correspond to position of a given variable on a template image for a given
field. The list of template images as well as instruction how to retrieve
them can be found in Papers I and II. The periods listed in Table 1 (click here)
were obtained using ANOVA statistics (Schwarzenberg-Czerny
1996). For each light curve we list also the intensity averaged V
magnitude, the full amplitude of light variations and the magnitude at
maximum light. For stars with multiple entries in Table 1 (click here) the
values of 
or 
show field-to-field differences
on the level of a few hundredth's of magnitude.
These differences reflect mostly some uncertainties of the zero
points of the photometry which were introduced by the particular
method of reduction. These uncertainties prevented us from combining
photometry obtained in different fields for the same variables.
For some of variables real and pronounced changes
of light curve amplitudes are observed. In fact Martin (1938)
was first to note such changes for several RR Lyr stars in 
Cen.
Table 2 (click here) gives equatorial coordinates for variables OGLEGC71-211.
We cross-correlated our list of variables with the Hogg (1973)
catalogue. The ID numbers from Hogg are listed in Cols. 2, 6 and 10 of
Table 2 (click here). For 33 variables we could not find their counterparts in
the Hogg catalogue. On the other hand we failed to obtain photometry for
several known variables which were present in the monitored fields.
The most common reason for such a failure was a presence of
badly saturated stellar images close to images of variables.
It has to be noted that our main goal was to look for
main sequence binaries. Therefore the duration of exposures was
not optimal for photometry of relatively bright variables
such as RR Lyr stars or Pop. II Cepheids.
In Fig. 1 (click here) we show light curves for variables whose luminosities
place them in the 
diagram on or near the level of the horizontal
branch of the cluster. Only one light curve was plotted for each of
variables although for many of them more than one light curve was obtained
(see Table 1 (click here)). The well known spread of average magnitudes of
Cen RR Lyr stars can be easily noted in Fig. 1 (click here).
No one of RR Lyr stars from our sample showed evidence for being a RRd
type variable (RRd stars pulsate simultaneously in the fundamental
and in the first overtone mode).
The sample of newly identified variables is dominated by objects with relatively low amplitudes. Moreover a large fraction of these stars have periods close either to 1/2 d or to 1/3 d. The period of OGLEGC162 is uncertain. The power spectrum for the light curve obtained in 1993 (field 5139B) shows peaks for periods 0.44 d, 0.28 d and 0.22 d. The data obtained in 1994 (field 5139BC) are best phased with period 0.268 d. The light curve of this variable is unstable on a time scale of days. Another new low-amplitude variable with unstable light curve is OGLEGC171 for which we adopted P=0.500 d. The period of this variable is rather firmly established - only one significant peak was detected in the power spectrum.
The light curves for 2 faintest and 6 brightest
variables from our sample are plotted in Fig. 2 (click here).
OGLEGC172 is a background RR Lyr star located well behind the
cluster. The nature of OGLEGC173 is less certain. The color of
this faint variable is rather red. With V-I=1.50
it is located about 0.5 mag to the red of upper main-sequence of
the cluster in the diagram. The variable was first erroneously
classified as a field RR Lyr star with a period of about 0.77 day and
therefore it was not included in Paper II with other faint variables from
field 5139D. The actual period of variability of OGLEGC173 is either 3.32
days or 6.64 days.
The possible classes of variables to which OGLEGC173 may belong include
the so called "spotted variables" and ellipsoidal variables.
The phased light curve presented in Fig. 2 (click here) shows a bump near
. This feature corresponds to a flare-like event which
occurred on 
. The data from that particular night
were discarded while determining a period of the variable.
Further observations are needed to solve questions about a nature
and membership status of OGLEGC173.
Figure 2: Phased light curves for 6 brightest and 2 faintest variables
from the present sample
Figure 3:
Period versus average V magnitude for bright pulsating variables
observed by OGLE in Cen. Objects classified as BL Her stars
or anomalous Cepheids are marked with open circles
Six bright stars whose light curves are plotted in Fig. 2 (click here)
have average magnitudes placing them above horizontal branch of
Cen. Variables V60 = OGLEGC103 and V61 = OGLEGC164
are classified as Pop. II Cepheids of BL Her subtype (eg. Nemec et
al. 1994). V52 = OGLEGC116 has a period 
. That value
is a bit shorter than the 0.75 day short period limit adopted for Pop. II
Cepheids (Wallerstein & Cox 1984). However,
luminosity of this star is appropriate for BL Her variables.
Properties of BL Her type variables were
recently discussed in some details by Nemec et al. (1994) and
Sandage et al. (1994).
Another BL Her star included in our sample is OGLEGC72 = V92.
Variables OGLEGC73 = V68 and OGLEGC174 = V84 are classified as
anomalous Cepheids (e.g. Nemec et al. 1994). The light curves
of OGLEGC72, OGLEGC73 and OGLEGC174 are presented in Fig. 1 (click here).
Bright variables OGLEGC123, OGLEGC156 and OGLEGC161
are new discoveries. For all these stars our data indicate periods
very close to 1 day which may explain why they were undetected in
the previous surveys.
Moreover, OGLEGC156 and OGLEGC161 show variations with full amplitudes
not exceeding 0.2 mag in the V-band.
We consider periods determined for these variables as preliminary.
Additional data are needed to settle this problem with confidence.
All 3 new variables belong probably either to BL Her stars or to
anomalous Cepheids.
In Fig. 3 (click here) we present "period" vs. "average magnitude" diagram for all but 2 faintest stars listed in Table 2 (click here).
ID | ID |  |  | ID | ID | | | ID | ID | | |
| OGLEGC | Hogg | deg | deg | OGLEGC | Hogg | deg | deg | OGLEGC | Hogg | deg | deg |
71 | - | 201.51720 | -47.36250 | 118 | 139 | 201.65717 | -47.45976 | 165 | 49 | 201.53207 | -47.63214 |
| 72 | 92 | 201.56204 | -47.35367 | 119 | 137 | 201.63132 | -47.45121 | 166 | 125 | 201.70382 | -47.68437 |
| 73 | 68 | 201.55338 | -47.32640 | 120 | 26 | 201.59838 | -47.44988 | 167 | - | 201.77620 | -47.78975 |
| 74 | 54 | 201.59794 | -47.31316 | 121 | - | 201.66737 | -47.44325 | 168 | 124 | 201.72642 | -47.65212 |
| 75 | 130 | 201.54138 | -47.22778 | 122 | - | 201.64628 | -47.43636 | 169 | 123 | 201.71274 | -47.62034 |
| 76 | 66 | 201.63813 | -47.37321 | 123 | - | 201.63128 | -47.43209 | 170 | 38 | 201.76341 | -47.60842 |
| 77 | 67 | 201.61904 | -47.31292 | 124 | 15 | 201.61282 | -47.41060 | 171 | - | 201.86329 | -47.79232 |
| 78 | 35 | 201.72260 | -47.37582 | 125 | 12 | 201.61321 | -47.40177 | 172 | - | 201.90180 | -47.77778 |
| 79 | 76 | 201.73895 | -47.33528 | 126 | 11 | 201.62727 | -47.38380 | 173 | - | 201.24356 | -47.60229 |
| 80 | 77 | 201.83780 | -47.36797 | 127 | 116 | 201.64777 | -47.46860 | 174 | 84 | 201.19769 | -47.49903 |
| 81 | - | 201.81487 | -47.35799 | 128 | 113 | 201.73459 | -47.52990 | 175 | 127 | 201.33068 | -47.47712 |
| 82 | 32 | 201.76454 | -47.36050 | 129 | 41 | 201.75577 | -47.51718 | 176 | 85 | 201.27703 | -47.39277 |
| 83 | 83 | 201.78576 | -47.35921 | 130 | 145 | 201.71342 | -47.51906 | 177 | - | 201.41680 | -47.58013 |
| 84 | 75 | 201.83222 | -47.31300 | 131 | - | 201.73556 | -47.50163 | 178 | 95 | 201.35352 | -47.48137 |
| 85 | 74 | 201.78016 | -47.29286 | 132 | - | 201.69624 | -47.50111 | 179 | 45 | 201.37848 | -47.45578 |
| 86 | 36 | 201.79213 | -47.25829 | 133 | 109 | 201.75638 | -47.49353 | 180 | 46 | 201.37591 | -47.43101 |
| 87 | 7 | 201.75377 | -47.23348 | 134 | - | 201.67875 | -47.43236 | 181 | 168 | 201.46996 | -47.53410 |
| 88 | 44 | 201.59329 | -47.57653 | 135 | 158 | 201.68880 | -47.51114 | 182 | 33 | 201.46532 | -47.48486 |
| 89 | 115 | 201.55115 | -47.57161 | 136 | 111 | 201.70414 | -47.47784 | 183 | 9 | 201.49921 | -47.43988 |
| 90 | 34 | 201.52988 | -47.55298 | 137 | 99 | 201.75887 | -47.46361 | 184 | 3 | 201.48478 | -47.43152 |
| 91 | 128 | 201.57385 | -47.50368 | 138 | 157 | 201.69355 | -47.45483 | 185 | 47 | 201.48627 | -47.40324 |
| 92 | 30 | 201.56631 | -47.49896 | 139 | - | 201.72635 | -47.45242 | 186 | - | 201.48890 | -47.37939 |
| 93 | 59 | 201.57670 | -47.49638 | 140 | 153 | 201.70686 | -47.43988 | 187 | 50 | 201.47532 | -47.45986 |
| 94 | 117 | 201.58286 | -47.48924 | 141 | 90 | 201.69048 | -47.43980 | 188 | 13 | 201.49339 | -47.42256 |
| 95 | - | 201.53425 | -47.50902 | 142 | 166 | 201.69154 | -47.43755 | 189 | 24 | 201.90982 | -47.57093 |
| 96 | - | 201.55463 | -47.43610 | 143 | 89 | 201.69145 | -47.43357 | 190 | 22 | 201.92110 | -47.56900 |
| 97 | 21 | 201.54647 | -47.43307 | 144 | 87 | 201.73941 | -47.42650 | 191 | - | 201.86920 | -47.52673 |
| 98 | 10 | 201.52913 | -47.41021 | 145 | 155 | 201.72345 | -47.41182 | 192 | 19 | 201.87601 | -47.46823 |
| 99 | 4 | 201.55384 | -47.40527 | 146 | 23 | 201.69363 | -47.41093 | 193 | 82 | 201.89860 | -47.44185 |
| 100 | 58 | 201.55432 | -47.40089 | 147 | 51 | 201.67741 | -47.40594 | 194 | 101 | 201.87641 | -47.49769 |
| 101 | 5 | 201.57633 | -47.38683 | 148 | - | 201.68216 | -47.38002 | 195 | 81 | 201.90295 | -47.41346 |
| 102 | 122 | 201.62631 | -47.55063 | 149 | - | 201.70715 | -47.46032 | 196 | - | 201.83594 | -47.39968 |
| 103 | 60 | 201.64876 | -47.54670 | 150 | 112 | 201.72602 | -47.50647 | 197 | 39 | 201.99892 | -47.57849 |
| 104 | 120 | 201.60633 | -47.54689 | 151 | 70 | 201.86581 | -47.56204 | 198 | 105 | 201.94182 | -47.54570 |
| 105 | 121 | 201.61735 | -47.53075 | 152 | - | 201.81882 | -47.55502 | 199 | 8 | 201.95184 | -47.47243 |
| 106 | 119 | 201.65951 | -47.52168 | 153 | 102 | 201.84206 | -47.50355 | 200 | 18 | 201.93784 | -47.41577 |
| 107 | 40 | 201.60228 | -47.51287 | 154 | 107 | 201.80847 | -47.51618 | 201 | 104 | 202.03213 | -47.56249 |
| 108 | - | 201.66516 | -47.50784 | 155 | - | 201.74977 | -47.45815 | 202 | - | 202.04299 | -47.39660 |
| 109 | 118 | 201.66890 | -47.50531 | 156 | - | 201.77052 | -47.45302 | 203 | - | 202.01447 | -47.35774 |
| 110 | 131 | 201.62518 | -47.49467 | 157 | 71 | 201.78352 | -47.46442 | 204 | 79 | 202.10412 | -47.49034 |
| 111 | - | 201.62582 | -47.47926 | 158 | 86 | 201.81315 | -47.43650 | 205 | 16 | 201.90671 | -47.62649 |
| 112 | 144 | 201.67926 | -47.47160 | 159 | 97 | 201.78529 | -47.42532 | 206 | 57 | 201.95551 | -47.61414 |
| 113 | 25 | 201.60624 | -47.47318 | 160 | 98 | 201.77429 | -47.44913 | 207 | 126 | 202.03345 | -47.67964 |
| 114 | 27 | 201.60839 | -47.47131 | 161 | - | 201.79136 | -47.45609 | 208 | - | 201.51848 | -47.44119 |
| 115 | - | 201.66501 | -47.46714 | 162 | - | 201.78882 | -47.38497 | 209 | - | 201.66053 | -47.55779 |
| 116 | 52 | 201.64648 | -47.46773 | 163 | 20 | 201.80842 | -47.46851 | 210 | 88 | 201.73296 | -47.42120 |
| 117 | 62 | 201.61070 | -47.46543 | 164 | 61 | 201.80816 | -47.45855 | 211 | 108 | 201.76947 | -47.49050 |
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