Updated Elements of Variable Stars in Sagittarius

W. Lemke
United States, Brookhaven

Received:   11.09.2023;   accepted:   14.12.2023
(E-mail for contact: potofcoppers@gmail.com)

Comments:


1. MinII = 13^m.71.

2. = ASAS J175927-3449.0.

3. MinII = 13^m.00. D = 0.14 P.

4. = OGLE-BLG-RRLYR-57089. M–m = 0.20 P.

6. MinII=14^m.55.

7. J=6^m.744, H=5^m.724, K=5^m.276 (2MASS).

8. M–m = 0.23 P.

9. = OGLE-BLG-RRLYR-62913. M–m = 0.20 P.

10. Note from the editor. Record in remarks to the GCVS: "IR Sgr VB B (A 13.6m; B 10", 220deg)". Despite that the designation IR Sgr was initially believed to refer to the brighter star (Gaia DR3 4076214200618375936) in the pair, the genuine RRAB is the fainter star Gaia DR3 4076214411158131968. Verified using ZTF data.
= PS1-3PI J183339.50-252042.2 = OGLE-BLG-RRLYR-62935.
M–m = 0.22 P.

11. = OGLE-BLG-RRLYR-63720. M–m = 0.45 P.

12. M–m = 0.17 P.

13. = OGLE-BLG-DSCT-14974.

14. J=6^m.813, H=5^m.880, K=5^m.469 (2MASS).

15. MinII = 15^m.92. D = 0.18 P.

Remarks:
I present updated elements of 16 variable stars in the constellation of Sagittarius. Variability types of several stars were identified incorrectly in the GCVS (Samus et al., 2017) and the VSX. Data was collected from the Zwicky Transient Facility (Bellm et al., 2019; Masci et al., 2019), the ASAS-SN (Kochanek et al., 2017), the ASAS database (Pojmanski et al., 2002), the Catalina survey (Drake et al., 2009) and the Gaia DR3 database (Gaia Collaboration et al., 2023). The observational series were analyzed using Peranso software to determine periods and light elements of the stars. Two new variables were discovered in the process and several suspected objects were confirmed to be variable. The coordinates are drawn from the Gaia DR3 (Gaia Collaboration et al., 2023).

Acknowledgements: This study became possible due to data from the databases including ASAS-SN, Zwicky Transient Facility (ZTF), ASAS, Catalina, 2MASS (Skrutskie et al., 2006) and Gaia DR3.

References:
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