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Table 1:

Optical observations of accreting white dwarfs used for construction of power spectra.

Target
Instr. Dates Mag. Time res., s Exp., ks Spin Period, s
XSS J00564+4548 RTT150 2005.10.19-23,26,28 14.9(V) 17-128 71.6 465
    2005.12.05,06 14.6(R)      
IGR J00234+6141 RTT150 2005.09.10-11,12.01 16.7(R) 60-70 37.6 561
    2005.12.10-11,2007.09.03 16.7(R)      
DO Dra RTT150 2007.04.24,27,28 14.7(R) 1 48 529
    2008.05.24-26,06.03 14.8(g') 1-8 39  
V1223 Sgr SALT 2008.05.13,2008.06.12 $\sim$13.3(B) 0.1 2.9 745
IGR J15094-6649 SAAO, 1m 2008.04.26-29 14.6(V) 7-8 14.9 809
IGR J16500-3307 SAAO, 1m 2008.04.27-28,05.04 15.9(V) 8-10 18.4 598*
  SAAO, 0.76m 2008.08.03-05 15.9(V)      
IGR J17195-4100 SAAO, 0.76m 2008.08.5-10 15.2(V) 8 32.3 1139*

Notes.  (*) - Here we use the optical pulsation period, which also may be the beat frequency instead of the true spin frequency of the white dwarf.


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