Table 2: Time series analysis for those objects in our sample where SiO periods can be established from our data. The SiO variability of GY Aql, an object considered as a semiregular star at the beginning of the survey, shows all the characteristics found in a typical Mira-type star. All other objects in our sample were not considered in this analysis because no periodicity could be found in the available data.
Name V1 Max./area   V2 Max./area   Optical or NIR Period
  P W D   P W D   P W D GCVS
o Cet 328.5/328.5 28/28 39/33   334.0/332.0 35/35 57/48   331.5 27 25 332.0
IK Tau1 475.5/471.0 94/100 29/15   453.2/452.0 100/99 -3/-20   467.5 129 2 470.0
TX Cam 540.0/542.0 66/69 82/67   532.3/533.0 98/106 64/77   542.5 79 44 557.4
R Cnc3,4 357.5/350.0 44/48 62/68   371.0/375.0 63/70 48/47   362.0 27 -6 361.6
R LMi2,3 375.0/376.5 36/36 42/47   375.0/378.0 34/38 46/59   374.5 27 -10 372.2
R Leo2 311.5/312.5 24/25 32/29   304.5/304.0 23/23 16/28   314.0 21 10 310.0
W Hya2,3,4 390.0/391.5 111/61 5/26   394.5/393.0 61/64 10/33   384.5 29 -8 361.0
U Her2,3,4 403.0/403.5 58/58 77/58   417.0/428.0 64/122 71/74   403.5 38 25 406.1
R Aql5 299.5/299.0 32/33 -5/3   299.0/296.0 40/45 -28/-10   279.5 17 0 284.2
R Aqr4 394.0/393.5 36/39 59/57   400.0/395.0 47/42 45/38   397.0 36 9 387.0
"                 395.5 42 38 387.0
R Cas2 440.5/436.5 51/51 57/55   434.5/435.0 40/44 43/31   434.5 40 12 430.5
IRC+100111 579.5/587.5 236/238 27/10   635.5/642.0 138/139 -36/-44   650.5 234 -55 660.0
GY Aql 460.0/455.0 54/49 40/38   459.5/457.0 51/51 52/54   461.5 76 -10 204.0
P: Peak of temporal power spectrum (days). W: Half power width of main peak (days). D: Delay with respect to Optical Max. (days). In bold face only if the delay is with respect to the NIR.
1 No optical data, curves and delays with respect to IR. 2 Possible low frequency component.
3 Possible high frequency component. 4 Possible harmonics. 5 Power spectrum with low SNR.

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