Table 1.
Open in new tab

Log of the observations.

HJD−2400000No. of framesTelescope
DY Peg, P = 0.072 926 492 d
54345.3938–54345.7439360IAC80
54346.4689–54346.7162435IAC80
54347.4898–54347.7409350IAC80
DH Peg, P = 0.255 510 37 d
54349.4951–54349.7057286IAC80
54352.4426–54352.6952410IAC80
54354.3792–54354.6757465IAC80
SW And, P = 0.442 266 d
54350.4678–54350.7399595IAC80
54351.4689–54351.7354535IAC80
54353.4203–54353.7441590IAC80
54822.2272–54822.4665320RCC
54829.2945–54829.4089180RCC
54830.3834–54830.430275RCC
54831.3594–54831.400380RCC
54832.2465–54832.3726205RCC
CU Com, |$P_0=0.543\,9036\,\text{d}, P_1=0.405\,6130$| d
54834.6136–54834.692350RCC
54871.6881–54871.7490a55IAC80
54873.6045–54873.7612135IAC80
54874.5278–54874.7652a165IAC80
56002.3537–56002.6375270RCC
56003.3173–56003.5793155RCC
56004.3384–56004.6196235RCC
56005.4446–56005.6223140RCC
56006.3127–56006.6300285RCC
56007.3018–56007.6325315RCC
56008.3011–56008.6224310RCC
56018.4911–56018.565235RCC
56019.3204–56019.6266280RCC
56020.3857–56020.6003150RCC
56021.2945–56021.351660RCC
56022.4480–56022.527580RCC
HJD−2400000No. of framesTelescope
DY Peg, P = 0.072 926 492 d
54345.3938–54345.7439360IAC80
54346.4689–54346.7162435IAC80
54347.4898–54347.7409350IAC80
DH Peg, P = 0.255 510 37 d
54349.4951–54349.7057286IAC80
54352.4426–54352.6952410IAC80
54354.3792–54354.6757465IAC80
SW And, P = 0.442 266 d
54350.4678–54350.7399595IAC80
54351.4689–54351.7354535IAC80
54353.4203–54353.7441590IAC80
54822.2272–54822.4665320RCC
54829.2945–54829.4089180RCC
54830.3834–54830.430275RCC
54831.3594–54831.400380RCC
54832.2465–54832.3726205RCC
CU Com, |$P_0=0.543\,9036\,\text{d}, P_1=0.405\,6130$| d
54834.6136–54834.692350RCC
54871.6881–54871.7490a55IAC80
54873.6045–54873.7612135IAC80
54874.5278–54874.7652a165IAC80
56002.3537–56002.6375270RCC
56003.3173–56003.5793155RCC
56004.3384–56004.6196235RCC
56005.4446–56005.6223140RCC
56006.3127–56006.6300285RCC
56007.3018–56007.6325315RCC
56008.3011–56008.6224310RCC
56018.4911–56018.565235RCC
56019.3204–56019.6266280RCC
56020.3857–56020.6003150RCC
56021.2945–56021.351660RCC
56022.4480–56022.527580RCC

aEpoch of the tie-in observations.

The source of the periods. DY Peg and CU Com: this work, DH Peg: Jones, Carney & Latham (1988), SW And: Liu & Janes (1989).

The comparison stars were GSC 1712−0984 (DY Peg), GSC 0565−1105 (DH Peg), GSC 1737−0809 (SW And) and GSC 1447−0968 (CU Com).

The check stars were GSC 1712−1246 (DY Peg), GSC 0565−1155 (DH Peg), GSC 1737−1139, GSC 1737−1194 (SW And) and GSC 1447−1184 (CU Com).

Table 1.
Open in new tab

Log of the observations.

HJD−2400000No. of framesTelescope
DY Peg, P = 0.072 926 492 d
54345.3938–54345.7439360IAC80
54346.4689–54346.7162435IAC80
54347.4898–54347.7409350IAC80
DH Peg, P = 0.255 510 37 d
54349.4951–54349.7057286IAC80
54352.4426–54352.6952410IAC80
54354.3792–54354.6757465IAC80
SW And, P = 0.442 266 d
54350.4678–54350.7399595IAC80
54351.4689–54351.7354535IAC80
54353.4203–54353.7441590IAC80
54822.2272–54822.4665320RCC
54829.2945–54829.4089180RCC
54830.3834–54830.430275RCC
54831.3594–54831.400380RCC
54832.2465–54832.3726205RCC
CU Com, |$P_0=0.543\,9036\,\text{d}, P_1=0.405\,6130$| d
54834.6136–54834.692350RCC
54871.6881–54871.7490a55IAC80
54873.6045–54873.7612135IAC80
54874.5278–54874.7652a165IAC80
56002.3537–56002.6375270RCC
56003.3173–56003.5793155RCC
56004.3384–56004.6196235RCC
56005.4446–56005.6223140RCC
56006.3127–56006.6300285RCC
56007.3018–56007.6325315RCC
56008.3011–56008.6224310RCC
56018.4911–56018.565235RCC
56019.3204–56019.6266280RCC
56020.3857–56020.6003150RCC
56021.2945–56021.351660RCC
56022.4480–56022.527580RCC
HJD−2400000No. of framesTelescope
DY Peg, P = 0.072 926 492 d
54345.3938–54345.7439360IAC80
54346.4689–54346.7162435IAC80
54347.4898–54347.7409350IAC80
DH Peg, P = 0.255 510 37 d
54349.4951–54349.7057286IAC80
54352.4426–54352.6952410IAC80
54354.3792–54354.6757465IAC80
SW And, P = 0.442 266 d
54350.4678–54350.7399595IAC80
54351.4689–54351.7354535IAC80
54353.4203–54353.7441590IAC80
54822.2272–54822.4665320RCC
54829.2945–54829.4089180RCC
54830.3834–54830.430275RCC
54831.3594–54831.400380RCC
54832.2465–54832.3726205RCC
CU Com, |$P_0=0.543\,9036\,\text{d}, P_1=0.405\,6130$| d
54834.6136–54834.692350RCC
54871.6881–54871.7490a55IAC80
54873.6045–54873.7612135IAC80
54874.5278–54874.7652a165IAC80
56002.3537–56002.6375270RCC
56003.3173–56003.5793155RCC
56004.3384–56004.6196235RCC
56005.4446–56005.6223140RCC
56006.3127–56006.6300285RCC
56007.3018–56007.6325315RCC
56008.3011–56008.6224310RCC
56018.4911–56018.565235RCC
56019.3204–56019.6266280RCC
56020.3857–56020.6003150RCC
56021.2945–56021.351660RCC
56022.4480–56022.527580RCC

aEpoch of the tie-in observations.

The source of the periods. DY Peg and CU Com: this work, DH Peg: Jones, Carney & Latham (1988), SW And: Liu & Janes (1989).

The comparison stars were GSC 1712−0984 (DY Peg), GSC 0565−1105 (DH Peg), GSC 1737−0809 (SW And) and GSC 1447−0968 (CU Com).

The check stars were GSC 1712−1246 (DY Peg), GSC 0565−1155 (DH Peg), GSC 1737−1139, GSC 1737−1194 (SW And) and GSC 1447−1184 (CU Com).

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