Circular No. 5378 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Postal Address: Central Bureau for Astronomical Telegrams Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. Telephone 617-495-7244/7440/7444 (for emergency use only) TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505 MARSDEN or GREEN@CFA.BITNET MARSDEN or GREEN@CFAPS2.SPAN EF PEGASI J. DeYoung and R. Schmidt, U.S. Naval Observatory, communicate: "With the 0.6-m reflector, 374 CCD images were made in the Kron- Cousins I band between Oct. 18.988 and 27.047 UT, during which time seven maxima were observed. A linear least-squares fit to these ob- servations and to the Kyoto report (IAUC 5371) yields the ephemeris HJDmax = 2448547.954 (+/- 0.006) + 0.08696 (+/- 0.00008)E. The pe- riod lies outside the period gap for cataclysmic variables. In the I band, EF Peg continues to decline in brightness at 0.1 mag/day, and the I superhump peak-to-peak amplitude has declined from 0.3 to 0.2 mag over the above interval; the maximum-minimum ratio is 0.3. Secondary 'humps' of amplitude < 0.1 mag in I at phase 0.6 were ob- served." Visual magnitude estimates by P. Schmeer, Bischmisheim, Germany: Oct. 22.74 UT, 11.7; 25.90, 12.2; 26.81, 12.4. GX 1+4 R. Sunyaev, M. Gilfanov, D. Barret, and F. Lebrun, on behalf of the GRANAT/SIGMA team (Space Research Institute, Moscow; Centre d'Etude Spatiale des Rayonnements, Toulouse; Service d'Astrophysique du CEA, Saclay), report: "During GRANAT observations of the Galac- tic Center region on Oct. 17-18 and 18-19, the hard x-ray flux (40- 70 keV) of GX 1+4 was found significantly higher than during previ- ous observations of this source obtained during Aug. 30-Oct. 10. The pulsation period (for the solar barycenter) was found to be 116.41 +/- 0.05 s, indicating further spin-down of the source (Pdot/P = 0.02 yrE-1), with respect to previously reported GRANAT observations in 1991 March and April (IAUC 5245)." NOVA SCUTI 1991 C. E. Woodward, University of Wyoming; and M. A. Greenhouse, National Air and Space Museum, Smithsonian Institution, write: "We obtained infrared spectra of N Sct 1991 on Sept. 29.10 UT with the Cerro Tololo Interamerican Observatory 1.5-m reflector (+ IRS spec- trometer). The Br-gamma H I emission line (2.166 microns) was re- solved with FWHM about 934 km/s and an observed flux of about 5.8 x 10E-17 erg cmE-2 sE-1. No [Si VII] coronal line emission at 2.474 microns was detected." 1991 October 30 Daniel W. E. Green