COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS NUMBER 826 Konkoly Observatory Budapest 1973 September 18 Veroffentlichungen der Remeis-Sternwarte Bamberg Astronomisches Institut der Universitat Erlangen-Nurnberg Band X, Nr. 107 Rosemary Hill Observatory, University of Florida Contribution No. 40 NEW SOUTHERN VARIABLE STARS On sky patrol plates taken at the Southern Station of the University of Florida, Gainesville and the Remeis-Sternwarte Bamberg, at the Mount John Observatory, New Zealand, the stars in the following list were found to be variable. The brightness of these stars were estimated by comparison with standard stars in the Harvard-Groningen Atlas, Selected Areas (1965, A. Brun and H. Vehrenberg). Finding charts, 1deg in declination, with south up, are also given. BV-Nr. RA Dec. Maximum Ampl. Remarks 1900.0 Brightness pg pg BV 1572 Pup = CoD -44d3424(10m) = CAP -44d1555(9.8m) 0.5m BV 1573 Pup = CoD -44d3450(10m) = CAP -44d1584(9.8m) 0.4 BV 1574 Pup 7h 55m 13s -38d43;3 11.0m 1.0 1 BV 1575 Pup = CoD -40d3763(9.3m) = CAP -40d2030(9.2m) 0.4 = HD 66436(F8) BV 1576 Vel = CoD -42d4345(10m) = CAP -42d2626(10.0m) 0.3 BV 1577 Vel = CoD -40d4603(9.1m) = CAP -40d2859(9.1m) 0.3 BV 1578 Vel = CoD -42d4977(9.1m) = CAP -42d3348(9.8m) 0.5 BV 1579 Vel = CoD -42d5032(9.8m) = CAP -42d3425(8.8m) 0.6 2 = HD 79101(A2) BV 1580 Pyx = CoD -32d6252(9.3m) = CAP -32d2570(9.4m) 0.8 BV 1581 Cen = CoD -47d6586(10m) 4.0^x 3 BV 1582 Cen = CoD -50d5778(9.9m) = CAP -50d4038(9.8m) 0.6 4 ^x Amplitude until plate limit (14m) Remarks: 1) BV 1574 is a Cepheid variable, whose ephemeris can be given as Max. = JD 2438442.354 + 15.565d E The following maxima were found: Maximum E O-C Maximum E O-C JD 2438442.354 0 0.000d JD 2439205.247 49 +0.208d 8739.551 19 +1.462 9562.256 72 -0.778 8816.335 24 +0.421 9935.885 96 -0.709 9143.419 45 +0.640 2440589.469 138 -0.855 9174.343 47 +0.434 1710.500 210 -0.504 Minimum occurs about phase 0.7. 2) BV 1579 is an Algol-type eclipsing binary. Only three minima were found: JD 2438443.399 2441394.906 2441689.080 3) BV 1581 is a Mira variable. The following maxima were found from a plot of magnitude estimates from all available patrol plates. In parenthesis after each maximum is given the number of points used to determine that maximum. JD 243 8473 (13) JD 244 0723 (6) 8793 (15) 1035 (9) 1721 (4) From these is obtained the ephemeris Max. = JD 2438793 + 325d E The variable is above the plate limit (14m) for approximately 120 days around the time of maximum Print 36 of the Canterbury Sky Atlas (1972, N.A. Doughty, C.D. Shane, and F.B. Wood), made from a plate exposed 120 days after maximum, may just barely show the variable. Since the limiting photographic magnitude of the atlas is stated to be magnitude 16, BV 1581 has an amplitude of at least six magnitudes. 4) BV 1582 is an Algol-type eclipsing binary, whose ephemeris is Min. = JD 2438471.404+ 1.776028d E The following minima were found: Minimum E O-C Minimum E O-C JD 2438407.549 -36 +0.082d JD 2438885.266 233 +0.047d 8471.404 0 0.000 8901.213 242 +0.010 8504.304 18.5 +0.079 9200.396 410.5 -0.067 8520.252 27.5 +0.008 9566.384 616.5 +0.059 8529.248 32.5 +0.084 9614.269 643.5 -0.009 8820.446 196.5 +0.052 2440735.809 1275 -0.031 8828.408 201 +0.022 1059.907 1457.5 -0.058 8844.382 210 +0.012 1092.823 1476 +0.002 8877.269 228.5 +0.043 The light curve shows a deep secondary eclipse. [FIGURE 1] [FIGURE 2] Bamberg, September 1973 W.H. SCHNEIDER Remeis-Sternwarte Bamberg and University of Florida Gainesville