CC BY
0Peremennye Zvezdy", Prilozhenie,
vol. 24, N 4 (2024)
New and Improved Light Elements for Twenty Suspected Variable Stars
E. V. Kazarovets
Institute ofAstronomy, Russian Academy of Sciences, Moscow, Russia ISSN 2221-0474 DOI: 10.24412/2221-0474-2024-24-4
Received: 13.06.2024; accepted: 17.09.2024
(E-mail for contact: helene@inasan.ru)
# Name Other Coord (J2000) TyP-e Max Min System Period Epoch (JD) iyp-e Sp Comment L.Curve Find.Chart Data
1 GSC 2.4 N8HZ016301 07 28 31.961 +23 08 53.40 EW 20.36 20.85 zr 0.241375 2459934.900 min Comm. 1 lc 01.jpg ch 01.png V01.txt
2 USN0-A2.0 1125-05275724 SE 07 39 31.472 +23 45 37.60 EW 16.10 16.21 zr 0.254513 2459153.022 min Comm. 2 lc 02.jpg ch 02.pns V02.txt
3 USN0-A2.0 1125-05281753 07 40 06.096 +23 49 28.86 DSCTC 17.74 17.82 zr 0.0592048 max Comm. 3 lc 03.jpg ch 03.pns V03.txt
4 GSC 7110-02470 07 44 58.222 -31 54 29.56 ELL 10.26 10.35 g 105.1 2460217.0 min WN6/WC4 Comm. 4 lc 04.jpg ch 04.pns V04.txt
5 GSC 7125-04392 08 10 18.098 -31 54 21.34 SR 13.94 16.29 g 433. 2459130. max C Comm. 5 lc 05.jpg ch 05.pns V05.txt
6 GSC 8163-01081 08 40 23.852 -51 26 46.33 SR 11.01 12.54 g 353. 2458778. max S6,8 Comm. 6 lc 06.jpg ch 06.png V06.txt
7 GSC 8613-00832 10 33 38.500 -59 01 22.13 EA 10.20 10.29 g 21.538 2459156.902 min Be Comm. 7 lc 07.jpg ch 07.pns V07.txt
8 USN0-A2.0 0225-09681745 10 52 02.392 -62 11 40.06 EA 15.45 15.92 V 2.04338 2458110.838 min Comm. 8 lc 08.jpg ch 08.pns V08.txt
9 GSC 9414-00812 11 06 04.903 -78 33 02.74 EA 14.36 14.59 g 3.45904 2460036.600 min Comm. 9 lc 09.jpg ch 09.pns V09.txt
10 USN0-A2.0 0075-02629942 11 08 14.750 -79 29 03.58 EW 15.54 15.71 g 0.334513 2460315.850 min Comm. 10 lc 10.jpg ch 10.png V10.txt
11 GSC 9418-02392 11 11 20.834 -79 17 10.16 EA 14.97 15.20 g 0.685782 2460074.462 min Comm. 11 lc 11.jpg ch 11.png V11.txt
12 USN0-A2.0 0150-08192388 11 12 23.571 -74 17 31.84 EW 15.37 15.72 g 0.317499 2460369.761 min Comm. 12 lc 12.jpg ch 12.pns V12.txt
13 GSC 9418-02402 11 14 01.321 -78 51 44.85 EA 15.12 15.62 g 1.97595 2460244.844 min Comm. 13 lc 13.jpg ch 13.png V13.txt
14 USN0-A2.0 0075-02673744 11 14 55.201 -77 45 35.10 DSCT 16.38 16.60 g 0.1270786 2460373.847 max Comm. 14 lc 14.jpg ch 14.pns V14.txt
15 GSC 3013-00129 11 21 48.837 +40 59 38.72 EW 12.84 13.02 zr 0.371493 2459434.654 min Comm. 15 lc 15.jpg ch 15.pns V15.txt
16 USN0-A2.0 0225-12978702 12 00 50.648 -60 26 33.65 EW 15.07 15.35 g 0.405436 2460100.702 min Comm. 16 lc 16.jpg ch 16.png V16.txt
17 GSC 8265-01229 13 31 36.156 -47 51 11.21 RVA 14.10 14.92 V 24.46 2460400.7 min Comm. 17 lc 17.jpg ch 17.pns V17.txt
18 USN0-A2.0 0900-07777357 14 44 24.479 +01 09 01.49 RRAB 19.12 19.87 zg 0.360017 2459478.612 max Comm. 18 lc 18.jpg ch 18.pns V18.txt
19 USN0-A2.0 0150-14048830 14 51 58.317 -72 36 40.92 EW 16.21 16.78 g 0.400008 2459758.370 min Comm. 19 lc 19.jpg ch 19.pns V19.txt
20 GSC 3481-01550 15 00 58.229 +46 55 36.09 EA 11.11 11.27 V 1.12963 2460436.680 min Comm. 20 lc 20.jpg ch 20.pns V20.txt
Comments:
1. = RAT J0728+2308. Min II = 20.76 zr. The sinusoidal type variability was suspected by Ramsay and Hakala (2005), no period.
2. = RAT J0739+2345. Min II = 16.20 zr. The variations with dips were suspected by Ramsay and Hakala (2005), no period.
3. = RAT J0740+2349. M - m = 0.45 P. The variability was suspected by Ramsay and Hakala (2005), no type or period.
4. = HD 62910 = HIP 037791 = WR 8 = LSS 731. Min II = 10.33 g; Min II - Min I = 0.45 P. O'Connell effect: Max II = 10.30 g. The variability with P = 114.6 d and without a type was suspected by Marchenko et al. (1998).
5. = IRAS 08083-3145 = CGCS 2095 = [W71b] 021-05. V = 12.09 - < 13.57. The ASAS-SN photometry in V and g bands, taken together, was used for period determination. Magnitudes in V were adjusted by +2 mag. The variability was discovered by Whitelock et al. (2006) with a type SR:, no period. The star was included in the ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with a type L without period.
6. = IRAS 08388-5116 = GCGSS 540 = He 4-51. V = 10.06 - 11.74. The variability was suspected by Van Eck et al. (2000). The star was included in the ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with a type L without period.
7. = HD 303004 = IRAS 10317-5845. Min II = 10.27 g, D = 0.05 P. In the reflection nebula GN 10.31.8 = BRAN 309D. The variability was suspected by Yudin and Evans (1998) according to observational data from literature.
8. = ASASSN-V J105201.92-621139.0. Min II = 15.63 V, D = 0.10 P. The variability was discovered by the ASAS-SN team (Jayasinghe et al. 2018) with the type EA and P = 4.0865791 d.
9. = 6771 in Chamaeleon I star-forming region. Min II = 14.58 g, D = 0.04 P. The short period variability was suspected by Carpenter et al. (2002).
10. = 12029 in Chamaeleon I star-forming region. Min II = 15.68 g. The short period variability was suspected by Carpenter et al. (2002).
11. = 19580 in Chamaeleon I star-forming region. Min II = 15.13 g, D = 0.12 P. The short period variability was suspected by Carpenter et al. (2002). The star is included in the ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with the type EW and P = 0.6857669 d.
12. = 22321 in Chamaeleon I star-forming region. Min II = 15.66 g. The short period variability was suspected by Carpenter et al. (2002). The star is included in the WISE catalogue (Chen et al. 2018) with the type EW and incorrect P = 0.3177814 d.
13. = 26688 in Chamaeleon I star-forming region. Min II = 15.20 g, D = 0.08 P. The variability with both short and long periods was suspected by Carpenter et al. (2002). The star is included in the WISE catalogue (Chen et al. 2018) with a type VAR and P = 1.9759512 d, as well as in the ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with the type EA and P = 3.951846 d.
14. = 29102 in Chamaeleon I star-forming region. The short period variability was suspected by Carpenter et al. (2002).
15. = ROTSE1 J112148.83+405938.0. Min II = 13.02 zr; zg = 13.29 - 13.47, Min II = 14.46 zg. The star was suspected by Kehoe et al. (2002) as pulsating variable candidate using NSVS photometric data (Wozniak et al. 2004), no period. Ferrante (2013) informed the VSX about the type EW and P = 0.371699 d for this variable. The object was included in the ZTF Catalogue of Variable Stars (Chen et al. 2020) with a type RSCVN and P = 0.1857474 d.
16. = Raf V102. Min II = 15.29 g. Twice shorter period and type DSCT are possible. Close fainter red companion (4" E-SE) and two brighter companions (15" N and 15" E). The variability was discovered by F. Hund in 2007 (RafV catalogue, 2005-2012), no type, period or magnitudes.
17. = UCAC4 211-079023. Min II = 14.75 V. The variability was discovered by Geffert et al. (2017), type SR without period. The star is included in the ASAS-SN Variable Stars Database (Jayasinghe et al. 2018) with the type EW and P = 24.4831 d.
18. = SDSS J144424.47+010901.5. M - m = 0.20 P; zr = 19.13 - 19.62. The ZTF photometry data combining zr and zg bands were used for period determination. The variability of RRAB type was suspected by Ivezic et al. (2000), no period. Sesar et al. (2017) confirmed type RRAB for the object PS1-3PI J144424.47+010901.5 and suggested incorrect P = 0.667676 d.
19. = Raf V123. Min II = 16.73 g. The variability was discovered by A. Paschke in 2007 (RafV catalogue, 2005-2012) with a type E, P = 0.3994 d, no magnitudes.
20. = TYC 3481-1550. Min II = 11.15, D = 0.08 P. The variability of this eclipsing star was reported by Hübscher (2017), no period and magnitudes. Remarks:
I continue studying behavior of stars from my archive of suspected variables, accumulated since 1990s. I set a goal to create the Second Supplement to the NSV catalogue (Kazarovets et al., 2022) of the archival stars before obtaining variability confirmation using CCD photometric data from contemporary sky surveys. For each of the archival stars, I acquire accurate positions and identifications with different catalogues, and I do my best to determine variability types and light elements. Then I select stars confirmed as variable by myself in order to transfer them to the General Catalogue of Variable Stars (GCVS) (Samus et al., 2017) via the next Name-Lists. Today 41% of 1000 studied stars comply with GCVS rules. In the current paper, I present 20 stars from confirmed 415 stars that proved to be variable. The study of the presented variables was made using the publicly available electronic archives of CCD observations of the Sky Patrol All-Sky Automated Survey for Supernovae (ASAS-SN) project (Shappee et al., 2014; Kochanek et al., 2017) and the Zwicky Transient Facility (ZTF) photometric data (Bellm et al., 2019; Masci et al., 2019) via the SNAD ZTF viewer (Malanchev et al., 2023). To find periods, I applied the WinEfk software provided by Dr. VP. Goranskij and the online light curve analysis tool developed by Dr. K.V. Sokolovsky. The coordinates of the stars were drawn from the Gaia DR3 catalogue (Gaia Collaboration, 2023).
References:
Bellm, E.C., Kulkarni, S.R., Graham, M.J., et al., 2019, Publ. Astron. Soc. Pacific, 131, No. 995, id. 018002 Carpenter, J.M., Hillenbrand, L.A., Skrutskie, M.F., Meyer, M.R., 2002, Astron. J., 124, No. 2, 1001 Chen, X., Wang, S., Deng, L., et al., 2018, Astrophys. J. Suppl. Ser., 237, Issue 2, id. 28 Chen, X., Wang, S., Deng, L., et al., 2020, Astrophys. J. Suppl. Ser., 249, Issue 1, id. 18 Ferrante, F., 2013, Private comm.
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Jayasinghe, T., Stanek, K.Z., Kochanek, C.S., et al., 2018, Mon. Not. Royal Astron. Soc., 486, No. 2, 1907 Kazarovets, E.V., Samus, N.N., Durlevich, O.V, 2022, Astron. Rep., 66, No. 7, 555 Kehoe, R., Akerlof, C. Balsano, R., et al., 2002, Astrophys. J., 577, No. 2, 845
Kochanek, C.S., Shappee, B.J., Stanek, K.Z., et al., 2017, Publ. Astron. Soc. Pacific, 129, No. 980, id. 104502 Malanchev, K., Kornilov, M.V., Pruzhinskaya, M.V., et al., 2023, Publ. Astron. Soc. Pacific, 135, No. 1044, id. 024503 Marchenko, S.V., Moffat, A.F.J., van der Hucht, K.A., et al., 1998, Astron. Astrophys., 331, No. 3, 1022 Masci, F.J., Laher, R.R., Rusholme, B., et al., 2019, Publ. Astron. Soc. Pacific, 131, No. 995, id. 018003 Ramsay, G., Hakala, P., 2005, Mon. Not. Royal Astron. Soc., 360, No. 1, 314
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