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IAUC 5665: FG Sge; V1333 Aql; N Cyg 1992

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IAUC number 

                                                  Circular No. 5665
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@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)


FG SAGITTAE
     D. Pollacco, Department of Physics and Astronomy, University
of St. Andrews, communicates:  "CCD imaging by S. A. Bell, R. W.
Hilditch, and D. L. Pollacco using the 1.0-m telescope at St.
Andrews University Observatory shows that FG Sge has been slowly
recovering from its recent unexpected deep minimum (IAUC 5604).
Observations on twelve nights since Oct. 19 show an apparently linear
increase of 0.015 mag/day (V) relative to five comparison stars
in the field (11' x 17').  The companion field star has not varied
over this period by more than 0.015 mag and is therefore probably
stable.  These results appear to be consistent with an ejection and
subsequent eclipse of material (cf. IAUC 5632) causing the abrupt
minimum.  Multicolor (BVRI) observations are available but await
absolute calibration for the field.  Observations are continuing
and we encourage spectroscopic observations."


V1333 AQUILAE
     S. A. Ilovaisky and C. Chevalier, Observatoire de Haute-
Provence, communicate:  "CCD photometry of V1333 Aql has been
obtained at Haute-Provence since it went into quiescence around mid-
June (IAUC 5551).  Observations were made with the 1.2-m telescope
on July 5-7 and 24-27, Aug. 4-8 and 18-24, and Sept. 1-3, 17-20,
and 29-30.  The source has remained in the quiescent state (V = 19)
throughout this entire interval.  However, in CCD frames taken on
Nov. 27, the object appears bright (V = 16.7), at least a magnitude
brighter than the average values (V = 17-18) seen during the last
outbursts in 1989, 1990, 1991, and 1992 (see Chevalier and
Ilovaisky 1991, A.Ap. 251, L11).  This confirms the start of a new
optical activity cycle coincident with the x-ray turn-on reported
in IAUC 5664.  Previous cycles have lasted about 150 days and
recurred every 300 days.  This one has started roughly on schedule."


NOVA CYGNI 1992
     D. Hanzl reports his additional UBV photometry of N Cyg 1992
(cf. IAUC 5623), obtained at the Nicholas Copernicus Observatory
and Planetarium in Brno with a 0.4-m reflector (comparison star HD
195664):  Oct. 14.745 UT, V = 10.14 +/- 0.03, B-V = -0.60 +/- 0.03,
U-B = -1.19 +/- 0.04; Nov. 7.724, 10.52 +/- 0.04, -0.63 +/- 0.03,
-1.58 +/- 0.02; Nov. 20.797, 10.62 +/- 0.11, -0.47 +/- 0.09, -1.74
+/- 0.07.


1992 December 2                (5665)            Daniel W. E. Green

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