Table 1: Set #1: ROTSE-I variables common with those in compilation of JK96.
Star Period (d) ${\varphi _{31}}$ [Fe/H] Star Period (d) ${\varphi _{31}}$ [Fe/H] Star Period (d) ${\varphi _{31}}$ [Fe/H]
XX And 0.722892 5.64487 -1.69 BB Eri 0.569875 5.28691 -1.32 $^{\sharp}$RX Cet 0.573449 5.82426 -1.2
SW Aqr 0.459272 4.96191 -1.14 RR Gem 0.397269 5.26756 -0.14 $^{\sharp}$AA Leo 0.598563 4.99218 -1.21
SX Aqr 0.535748 4.91896 -1.55 VX Her 0.455332 4.92637 -1.21 $^{\sharp}$VY Lib 0.533404 5.61394 -1.06
BO Aqr 0.693934 5.66499 -1.52 VZ Her 0.440325 4.86611 -0.8 $^{\sharp}$V445 Oph 0.397044 5.73612 0.01
BR Aqr 0.481782 5.44115 -0.6 SV Hya 0.478595 4.90845 -1.43 $^{\sharp}$AR Per 0.425531 5.69689 -0.14
CP Aqr 0.463398 5.40211 -0.5 ST Leo 0.477959 5.09023 -0.98 $^{\sharp}$RY Psc 0.529497 5.53738 -1.18
DN Aqr 0.633917 5.63168 -1.36 TV Leo 0.672885 5.26225 -1.86 $^{\sharp}$V440 Sgr 0.477566 5.19756 -1.21
AA Aql 0.361821 5.08321 -0.27 V LMi 0.543888 5.35767 -0.93 $^{\sharp}$UU Vir 0.475606 5.34802 -0.6
TZ Aur 0.391639 5.15205 -0.62 U Lep 0.581236 4.86869 -1.67 $^{\sharp}$AV Vir 0.656954 5.77266 -1.02
TW Boo 0.532293 5.18551 -1.15 TT Lyn 0.597413 5.43315 -1.5 $^{\sharp}$FH Vul 0.405541 4.41535 -0.61
W CVn 0.551739 5.32863 -0.91 IO Lyr 0.577164 5.33299 -1.1 $^{\ast}$ V341 Aql 0.578302 5.08152 -0.92
RR Cet 0.552996 5.33238 -1.29 ST Oph 0.450383 5.14435 -1.02 $^{\ast}$ RZ Cet 0.510606 5.25459 -1.24
S Com 0.586574 5.30487 -1.64 V452 Oph 0.557153 5.02819 -1.45 $^{\ast}$ BK Dra 0.592080 5.07697 -1.83
DX Del 0.472685 5.77432 -0.32 AV Peg 0.390106 5.72178 0.08 $^{\ast}$ AN Ser 0.522001 6.06785 0.09
SU Dra 0.660300 5.44729 -1.56 AT Ser 0.746538 5.65698 -1.8 $\cdots$ $\cdots$ $\cdots$ $\cdots$
RX Eri 0.587272 5.67619 -1.07 $^{\sharp}$X Ari 0.650811 4.86683 -2.1 $\cdots$ $\cdots$ $\cdots$ $\cdots$
Notes: A pound sign in the "Star'' column indicates a star with a bad quality light curve, i.e. insufficient-phase-coverage or noisy light curves. Asterisks in the "Star'' columns indicate the the peculiar variables of JK96; the column "[Fe/H]'' shows spectroscopic iron abundance as it was given in JK96.

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