New Elements of 42 Southern Variables

A. V. Khruslov
Tula, Russia

Received:   30.03.2011;   accepted:   3.06.2011
(E-mail for contact: khruslov@bk.ru)

Comments:


1. The variability of TYC 6433 1366 1 was reported by Pojmanski (2002). The ASAS-3 catalog lists the variable as an EC/RRC star with the wrong period of 0.61105 d. I reinvestigated the star using the currently available ASAS-3 data and found it to be an EW eclipsing binary with a shorter period. MinII = 12.75.

2. The variability of GSC 7046-01634 was discovered by Pojmanski (2002). The ASAS-3 catalog lists the variable as a Cepheid (DCEP-FU) with the wrong period of 1.2215 d. I reinvestigated the star using the currently available ASAS-3 data and found it to be an RRAB variable star. The period suggested by Pojmanski (2002) is a one-day alias of the real one (see the Table). M–m = 0.22 P. J–H = 0.168 (2MASS). The period probably is somewhat variable.

3. The variability of GSC 7068-00307 was reported by Pojmanski (2002). The ASAS-3 catalog lists the variable as an RRC: star with the wrong period of 0.270632 d. I reinvestigated the star using the currently available ASAS-3 data and found it to be an RRAB variable star. The period suggested by Pojmanski (2002) is a one-day alias of the real one (see the Table). M–m = 0.20 P. J–H = 0.329 (2MASS). Blazhko effect with the period P = 40.5 d.

4. The variability of DQ Lup was discovered by McLeod and Swope (1941). The variable was classified in the GCVS as an RR star with the wrong period of 0.31582 d. According to ASAS-3 data, it is an RRC star. The period suggested by GCVS is a one-day alias of the real one (see the Table). M–m = 0.42 P. J–H = 0.153 (2MASS).

5. The variability of UZ Lup was discovered by Mohr (1929). The variable was classified in the GCVS as an RR: star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.20 P. J–H = 0.325 (2MASS).

6. The variability of GSC 6170-00445 was reported by Pojmanski (2002). The ASAS-3 catalog lists the variable as a DSCT star with the wrong period of 0.10098 d. I reinvestigated the star using the currently available ASAS-3 data and the ROTSE-I/NSVS data. The period suggested by Pojmanski (2002) is a one-day alias of the real one (see the Table). M–m = 0.39 P. J–H = 0.149 (2MASS).

7. The variability of DO Lib was discovered by Hanley (1942). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 and ROTSE-I/NSVS data, it is an RRAB star. M–m = 0.24: P. J–H = 0.313 (2MASS).

8. The variability of DR Lib was discovered by Hanley (1942). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.22: P. J–H = 0.247 (2MASS).

9. The variability of EO Lib was reported by Hanley (1942). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 and ROTSE-I/NSVS data, it is an RRAB star. M–m = 0.21 P. J–H = 0.281 (2MASS). The tabulated amplitude is too low: ASAS-3 measured the combined brightness of two stars, GSC 6191-01124 and GSC 6191-01108; the NSVS amplitude is still lower than the ASAS-3 one, three stars (with the addition of GSC 6191-01128) were measured there.

10. BO Sco, an IN: type star (Orion variable) in the GCVS, where the information was based on Satyvoldiev (1982), is actually a semiregular pulsating star (SRA type) according to ASAS-3 data. J–H = 1.025 (2MASS).

11. The variability of AW Sco was discovered by Leavitt (1904). No light elements have been published to the present. According to ASAS-3 data, it is an RRAB star. M–m = 0.18 P. J–H = 0.188 (2MASS).

12. The variability of FL Sco was reported by Swope (1928a). The variable was classified in the GCVS as an RR: star without light elements. According to ASAS-3 data, it is an eclipsing variable star (EW type). MinII = 13.5.

13. The variability of KN Sco was discovered by Swope (1928b). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 data, it is an eclipsing variable star (EW type). MinII = 14.1. The close faint companion USNO-A2.0 0525-26382756 probably makes the ASAS amplitude too low.

14. The variability of V610 Sco was reported by Swope (1943). The variable was classified in the GCVS as an eclipsing variable (E type) without light elements. According to ASAS-3 data, it is an EB star. MinII = 13.0.

15. V428 Sco, an I type star (poorly studied irregular variable) in the GCVS, where the information was based on Swope (1936), is actually a semiregular pulsating star according to ASAS-3 data. Its colour index J–H = 0.665 (2MASS) and spectral type K0–K2 (Cieslinski et al. 1998) suggest the SRD type. The variable has two close faint companions, 2MASS 17563007-3708053 and 2MASS 17562951-3708134.

16. The variability of CP Pav was discovered by Shapley et al. (1939). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.27 P. J–H = 0.306 (2MASS). The close faint companion 2MASS 18095102-5700544 possibly makes the ASAS amplitude somewhat too low.

17. The variability of V3801 Sgr was discovered by Hoffleit (1972). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 data, it is an EW type star. MinII = 13.95.

18. The variability of V3810 Sgr was reported by Hoffleit (1972). The variable was classified in the GCVS as an EW: type star without light elements. I confirm the eclipsing nature of this variable and suggest EW type according to ASAS-3 data. MinII = 13.4. The close faint companion USNO-A2.0 0675-25382928 probably makes the ASAS amplitude too low.

19. The variability of V3820 Sgr was reported by Hoffleit (1972). The variable was classified in the GCVS as a Cepheid (CEP:) with the possible period P=14: d. I confirm the pulsating nature of this variable (CEP type) according to ASAS-3 data. M–m = 0.35 P. J–H = 0.486 (2MASS).

20. The variability of V3335 Sgr was discovered by Plaut (1971). The variable was classified in the GCVS as an SRB: star (or maybe a Cepheid or an RV Tau variable) without light elements. According to ASAS-3 data, it is definitely an RVA star. J–H = 0.313 (2MASS). Probably a double star on the Palomar images.

21. The variability of V3824 Sgr was discovered by Hoffleit (1972). The variable was classified in the GCVS as an RR: type star without light elements. According to ASAS-3 data, it is an RRAB star. J–H = 0.148 (2MASS). Observations are also satisfied by a twice shorter period, 0.30604 d, so that the type becomes RRC.

22. V1610 Sgr, a CEP: star (possible period P < 0.5 d) in the GCVS, where the information was based on Ponsen (1955), is actually a semiregular pulsating star (SR) according to ASAS-3 data. J–H = 0.942 (2MASS). Probably it can be identified with IRAS 18242–2711.

23. V3833 Sgr, an LB: star (slow irregular variable, spectral type M0:) in the GCVS, where the information was based on Hoffleit (1972), is actually an SR star according to ASAS-3 data. J–H = 0.968 (2MASS).

24. The variability of V1899 Sgr was discovered by Hoffleit (1961). The variable was classified in the GCVS as an RV star without light elements. The ASAS-3 catalog lists the star as a MISC variable with the period of 52.880001 d. I reinvestigated the star using the currently available ASAS-3 data and found it an RVA variable star with a twice longer period. J–H = 0.444 (2MASS). The shape of the light curve varies, so that the primary minimum becomes the secondary one and vice versa.

25. The variability of V2363 Sgr was discovered by Hoffleit (1965). The variable was classified in the GCVS as an LB: star (slow irregular variable), of the spectral type M7. According to ASAS-3 data, it is a semiregular pulsating star. J–H = 1.179 (2MASS). IRAS 18295–2316.

26. The variability of V3597 Sgr was reported by Plaut (1971). The variable was classified in the GCVS as a Mira star (M:) with the period of P = 193: days. According to ASAS-3 data, the period from the GCVS is wrong. J–H = 0.835 (2MASS). IRAS 18316–3203. There is a close faint companion, USNO-B2.0 0579-0941562.

27. The variability of CX Pav was discovered by Shapley et al. (1939). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.17 P. J–H = 0.156 (2MASS).

28. The variability of V3687 Sgr was reported by Plaut (1971). The variable was classified in the GCVS as an SR star without light elements. According to ASAS-3 data, it is a semiregular pulsating star (SRA). J–H = 0.846 (2MASS). IRAS Z18349–3643.

29. The variability of CZ Pav was discovered by Shapley et al. (1939). The variable was classified in the GCVS as an RR star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.18 P. J–H = 0.036 (2MASS). Because of the close companion 2MASS 18511965–5850581, the ASAS amplitude is probably too low.

30. The variability of OO Pav was reported by Gessner and Meinunger (1974). The variable was classified in the GCVS as an L-type star (slow irregular variable). The ASAS-3 catalog lists the star (ASAS J185758–7150.9) as a MISC variable with the wrong period of P = 62.761505 d. I reinvestigated the star using the currently available ASAS-3 data and found it a semiregular pulsating star (SRA) with a twice longer period. J–H = 0.723 (2MASS).

31. The variability of V2153 Sgr was reported by Hoffmeister (1963a). The variable was classified in the GCVS as an EB type star without light elements. According to ASAS-3 data, it is an eclipsing variable star (EW type). MinII = 13.8.

32. V2166 Sgr, an IS: type star (variable star with rapid variations) in the GCVS, where the information was based on Hoffmeister (1963a), is actually an eclipsing variable star (EA type) according to ASAS-3 data. D = 0.15 P. MinII = 13.8. A twice shorter period is not excluded.

33. The variability of V2184 Sgr was discovered by Hoffmeister (1963a). The variable was classified in the GCVS as an EA-type star without light elements. I confirm the eclipsing nature of this variable (EA type) according to ASAS-3 data. D = 0.024 P. This is an eccentric binary system, the phase of MinII being 0.768 P.

34. The variability of V2192 Sgr was discovered by Hoffmeister (1963a). The variable was classified in the GCVS as an RR type star without light elements. According to ASAS-3 data, it is an eclipsing variable star (EW type). MinII = 14.2.

35. The variability of V2202 Sgr was reported by Hoffmeister (1963a). The variable was classified in the GCVS as an RR type star without light elements. According to ASAS-3 data, it is an RRAB star. J–H = 0.230 (2MASS).

36. The variability of QY Pav was discovered by Gessner and Meinunger (1974). The variable was classified in the GCVS as an eclipsing variable star (E type). No period is tabulated there, the time of minimum is given as HJD 2436785.247. I confirm the eclipsing nature of this variable (EW type) according to ASAS-3 data. MinII = 14.5.

37. The variability of FY Pav was discovered by Gessner and Meinunger (1974). The variable was classified in the GCVS as an eclipsing variable star (EA:/SD:), with the times of minima MinI = JD2436808.433, MinII = JD2436784.37. I confirm the eclipsing nature of this variable (EA type) according to ASAS-3 data. MinII = 13.9. D = 0.052 P.

38. The variability of V2223 Sgr was reported by Hoffmeister (1963a). The variable was classified in the GCVS as an RR type star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.30: P. J–H = 0.069 (2MASS).

39. The variability of V2227 Sgr was reported by Hoffmeister (1963a). The variable was classified in the GCVS as an RR type star without light elements. According to ASAS-3 data, it is an RRAB type star. M–m = 0.15: P. J–H = 0.191 (2MASS). There is a close faint companion, 2MASS 20032409–4009044.

40. The variability of V2240 Sgr was reported by Hoffmeister (1963a). The variable was classified in the GCVS as an RR type star without light elements. According to ASAS-3 data, it is an RRAB type star. J–H = 0.224 (2MASS). The ASAS measured combined brightness of two stars, V2240 Sgr = GSC 7960–00866 = 2MASS 20105204–4337181 and 2MASS 20105250–4337238, so the amplitude is too low.

41. The variability of V2264 Sgr was reported by Hoffmeister (1963a). The variable was classified in the GCVS as an RR type star without light elements. According to ASAS-3 data, it is an RRAB star. J–H = 0.265 (2MASS).

42. The variability of V338 Pav was reported by Hoffmeister (1963b). The variable was classified in the GCVS as an RR: type star without light elements. According to ASAS-3 data, it is an RRAB star. M–m = 0.24 P. J–H = 0.278 (2MASS).

Remarks:
I present my investigation of 42 known variable stars based on ASAS-3 (Pojmanski 2002) and ROTSE-I (Wozniak et al. 2004) data. These observations were analyzed using the period-search software developed by Dr. V.P. Goranskij for Windows environment. For the studied stars, previously suggested light elements and/or variability types were found to be wrong. The coordinates were drawn from the GCVS, Tycho-2 or 2MASS catalogs.

References:
Cieslinski, D., Steiner, J.E., Jablonski, F.J., 1998, Astron. Astrophys. Suppl., 131, 119
Gessner, H., Meinunger, I., 1974, Veröff. Sternwarte Sonn., 6, 249
Hanley, C.M., 1942, Harvard Observ. Annals, 109, 15
Hoffleit, D., 1961, Astron. J., 66, 188
Hoffleit, D., 1965, Astron. J., 70, 307
Hoffleit, D., 1972, IBVS, No. 660
Hoffmeister, C., 1963a, Veröff. Sternwarte Sonn., 6, 1
Hoffmeister, C., 1963b, Astron. Nachr., 287, 59
Leavitt, H.S., 1904, Harvard Observ. Circ., 90, 1
McLeod, N.W., Swope, H.H., 1941, Harvard Observ. Bull., 915, 29
Mohr, J., 1929, Harvard Observ. Bull., 866, 18
Plaut, L., 1971, Astron. Astrophys. Suppl., 4, 75
Pojmanski, G., 2002, Acta Astron., 52, 397
Ponsen, J., 1955, Leiden Annals., 20, 383
Satyvoldiev, V., 1982, Perem. Zvezdy Prilozh., 4, 127
Shapley, H., Boyce, E.H., Boyd, C.D., 1939, Harvard Observ. Annals, 90, 239
Swope, H.H., 1928a, Harvard Observ. Bull., 857, 1
Swope, H.H., 1928b, Harvard Observ. Bull., 862, 29
Swope, H.H., 1936, Harvard Observ. Annals, 90, 207
Swope, H.H., 1943, Harvard Observ. Annals, 109, 41
Wozniak, P.R., Vestrand, W.T., Akerlof, C.W., et al., 2004, Astron. J., 127, 2436