COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 2292 Konkoly Observatory Budapest 1983 March 10 HU ISSN 0374-0676 PHOTOELECTRIC TIMES OF MINIMA OF ECLIPSING BINARIES Photoelectric V-filter observations of selected eclipsing binaries were continued with the 40-cm f/18 Cassegrain reflector at the Blue Mountain Observatory during the 1982 observing season. The observing procedure was identical to that described in Margrave et al. (1978). Following past practice, least-squares parabolic fits were made to the observations. Table I contains the resultant Heliocentric Julian Date Table I. Heliocentric Times of Minima Star Hel. JD - 2,440,000 E O-C Remark KO Aql 5209.7844+ 0.0003 1160 +0.0082d P RZ Cas 5204.7352+ 0.0008 12825 -0.0016 P 5217.8828+ 0.0008 12836 -0.0017 P TV Cas 5256.8056+ 0.0002 2020 +0.0067 P TW Cas 5207.8303+ 0.0001 2240 -0.0028 P PV Cas 5164.5753 1962 -0.0022 S 5165.4760 1963 +0.0022 P 5253.8509+ 0.0004 2013 -0.0008 S XX Cep 5206.7625+ 0.0008 1569 +0.0088 P 5220.7876+ 0.0004 1575 +0.0099 P SW Lac 5201.7407+ 0.0005 5431 -0.0063 S 5203.8264+ 0.0009 5438 -0.0053 P 5204.7892+ 0.0006 5441 -0.0046 P AT Peg 5219.8562+ 0.0005 4199 +0.0064 P (minus 2,440,000) for each eclipse along with its probable error, cycle number E, and O-C value. The data for the first two eclipses of PV Cassiopeiae were kindly supplied by Dr. Alvaro Gimenez (1982). The letters P and S in the Remark column denote a primary or secondary eclipse, respectively. The references for the ephemerides used to calculate the O-C values are given in Table II. Table II. Ephemerides References Star Reference KO Aql Margrave (1980) RZ Cas Herczeg and Friboes-Conde (1974) TV Cas Margrave (1980) TW Cas Margrave (1980) PV Cas Gimenez and Margrave (1982) XX Cep SAC 53 SW Lac Faulkner and Bookmyer (1978) AT Peg Margrave (1981) The residuals for RZ Cassiopeiae appear to have reversed the trend towards more negative values that was exhibited during the preceding two seasons. The residuals for XX Cephei continue to become more positive, which indicates that the period given in SAC 53 needs to be increased. The quadratic elements for AT Pegasi cited in Table II provide much smaller residuals for the eclipse time given here and those given in the previous notes from this observatory than do the quadratic elements given in SAC 54. In the case of the AT Pegasi eclipse reported here the SAC 54 quadratic elements yield O-C = -0.0821d. Those who plan to observe this system should make allowance for this discrepancy if they use the SAC 54 quadratic elements. The author would like to acknowledge the financial support provided by a University of Montana Research Grant, which made it possible to secure the Blue Mountain observations reported herein. THOMAS E. MARGRAVE Blue Mountain Observatory University of Montana Missoula, Montana 59812 USA References: Faulkner, D. R. and Bookmyer, B. B. 1978, IBVS No. 1503. Gimenez, A. 1982, private communication. Gimenez, A. and Margrave, T. E. 1982, Astr. J., 87, 1233. [BIBCODE 1982AJ.....87.1233G ] Herczeg, T. and Friboes-Conde, H. 1974, Astr. and Ap., 30, 259. [BIBCODE 1974A&A....30..259H ] Margrave, T. et al. 1978, IBVS No. 1478. Margrave, T. 1980, IBVS No. 1869. Margrave, T. 1981, IBVS No. 1930. Rudnicki, K. 1982, Supplemento ad Annuario Cracoviense No. 53, Krakow. Rudnicki, K. 1983, Supplemento ad Annuario Cracoviense No. 54, Krakow, p. 102.