COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS NUMBER 726 Konkoly Observatory Budapest 1972 October 16 NEW RESULTS ON KNOWN VARIABLES IN SAGITTARIUS In a recent publication on variable stars in Sagittarius Plaut (1971) noted several long period variables for which a definitive choice between two alternative periods was not possible on the basis of his available plate material. A few of these stars are in an area overlapping the field of the Maria Mitchell Observatory plates. I therefore suggested to Carol Day that she examine these stars and combine her own observations with the published data, thereby seeking more definitive solutions. Also included in our summer 1972 program were other previously published variables for which different authors had obtained discordant results, or stars for which errors in the General Catalogue of Variable Stars had come to my attention, and a few stars still listed only in the Catalogue of Suspected Variables. A summary of the results is given in the Table, where previously published periods, or types (if now revised) are noted together with the new or revised periods. The initials in the last column indicate the recent investigator (CD, Carol Day; BH, Barbara Hatfield; PK, Pamela Knight; and DH, Dorrit Hoffleit) while the number refers to a footnote. [FIGURE 1] For six of the variables for which no finder charts have previously been published, such charts are given here. The stars marked A, B or C are identified as follows: MW Sgr C CoD -27d13160 V1709 B BD -19d5136 V 929 A CoD -31d15485 S 4309 A CoD-30d16079 B 15488 B 16088/9 C 15494 GS Sgr Chart area 5'x5' V1703 B BD -18d5031 Miss Carol Day and Miss Pamela Knight were summer NSF Undergraduate Research Participants, while Miss Barbara Hatfield was employed under NSF Grant GP-30065. We are grateful to the National Science Foundation for this support and encouragement. 8 October 1972 DORRIT HOFFLEIT Maria Mitchell Observatory Nantucket, Mass., U.S.A. References Innes, R., 1917, Union Observatory Cir. No. 37 Plaut, L., 1971, Astron. and Astrophys. Supp. Series, 4, No. 2. [BIBCODE 1971A&AS....4...75P ] TABLE Revised Results for Variables in Sagittarius ---------------------------------------------------------------------- Var. Previously Published Revised Elements Span of Note Sgr Periods Epochs ---------------------------------------------------------------------- MW 260,207,208.3,208,5 36085+204n+ +15sin4.5(n+42) 110 CD V929 196,8,400 35687+194.5n 122 CD V932 225,227.5,149 28422+225n 98 CD V938 220.7,219.5,137 19575+138n 129 CD,1 V1293 153,154.8,272 27711+155n 88 CD V1703 207,312 26120+206n 75 CD,2 V1709 212, UG 26160+210.8n 73 CD,3 V1835 173,262 27635+262n 80 CD V1836 242,244,301.5, 27635+244n 57 CD V1919 162,162.8,189.4 27635+162n 58 CD V2032 UG? 1250? 36720+229.5n 75 DH,4 V2368 194 26570+193.8n 90 DH,5 V2378 312 36750+312n 44 CD V2383 UG 25850+188.5n 94 DH,6 V2565 300: 27630+305:n 45 PK,7 DH117b 320 26120+320:n 17 PK,7 54025 28.14 37826+28.14n BH,8 54309 - 37100+422n 53 PK GS - SR~360days?. PK,9 ---------------------------------------------------------------------- Notes to Table 1. V 938 Sgr. A period of 220 days is still not precluded. 138 days is preferred because it appears to represent the early observations by Innes slightly better. No Nantucket observations available for this star. 2. V 1703 Sgr. The period of 207 days given for this star in A.J., 62, 121 1957 (HV12398) is essentially correct. The period of 312 days given in the General Catalogue refers to V 2378 Sgr. The confusion is attributed to the crude positions given by Hartsock in her provisional paper in AAVSO Abstracts, Fall 1964. 3. V1709 Sgr. The type UG listed in the General Catalogue refers to V2383. Same comment as for V1703 Sgr. 4. V2032 Sgr. The previously published type and period depended upon only four observed maxima with a minimum separation of 2500 days. Nantucket plates for 1957-72 reveal the revised period which also satisfies the earlier Harvard observations. Mira Type. 5. V2368 Sgr. New measures have been added because the period given in A.J., 70, 307, 1965 (star 17) has been omitted from the General Catalogue. 6. V2383 Sgr. Because of crude positions this star was belived to be V1709 Sgr (q.v.). 7. V2565 Sgr and DH 117b (See IBVS 617 and 660). These two stars were re-examined to avert any possible confusion between two stars close together both in position and period. 8. 54025. HV 9396. The period for this W Virginis type star, given in A.J., 69, 301, 1964 (Star 3) has been confirmed by further observations for the interval JD 38169-41219. 9. GS Sgr. Probably semi-regular. No satisfactory period found. Cycles of about a year, more frequently at maximum than minimum. Miss Knight finds that a period of 180 days seems to represent a high percentage of the observations. However, the duration of maximum or of minimum is sometimes 150 days. Doubling her period gives no improvement as the period is too close to one year.