Central Bureau for Astronomical Telegrams
IAUC 4573: N Vul 1987; 1988 EG; B2 0927+35
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Read IAUC 4574
Circular No. 4573
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
TWX 710-320-6842 ASTROGRAM CAM Telephone 617-495-7244/7440/7444
NOVA VULPECULAE 1987
R. M. Wagner, Ohio State University; and J. S. Gallagher,
Lowell Observatory, write: "Spectrophotometric observations obtained
with the OSU Image-Dissector Scanner (range 370-640 nm, resolution
1 nm) and the Perkins 1.8-m telescope on Mar. 13.5 UT show
emission lines of [O I] (630.0, 636.3, 557.7 nm), [N II] (575.5
nm), [O III] (500.7, 495.9, 436.3 nm), H-beta, and H-gamma. Photometry from
the spectrum gives magnitude V about 17. Wavelength centroids of the
emission lines are blueshifted about 1-1.5 nm with respect to their
nominal rest wavelengths, consistent with the formation of an
optically thick dust shell (IAUC 4557) which is obscuring the
redshifted part of the ejecta."
Photovisual magnitude estimate (cf. IAUC 4566) by R. Royer,
Wrightwood, CA: Mar. 24.51 UT, 15.5.
1988 EG
E. Bowell reports that CCD observations on 1988 Mar. 24 and
26 by S. J. Bus and C. J. Cunningham at the 1.8-m Perkins telescope,
Lowell Observatory, appear to indicate that the newly discovered
Apollo-type asteroid 1988 EG has a rotation period of 4.27 hr, a
peak-to-peak lightcurve amplitude of slightly less than 0.2 mag,
and exhibits three pairs of extrema per rotation.
B2 0927+35
J. Machalski, Cracow Observatory; and F. La Franca, Padova
Observatory, communicate: "The faint object identified with this
radio source (Allington-Smith et al. 1982, MNRAS 201, 331) has
brightened by at least 2 mag. A change of its 1.4-GHz flux was
noticed by Machalski and Rys (in preparation); subsequently, the
high-frequency spectrum was observed by Machalski and Inoue with
the Nobeyama 45-m radio telescope in 1988 Feb. at 10 and 40 GHz. A
very bright radio component has been deduced at mm wavelengths.
CCD photometry obtained with the 1.82-m telescope at Cima Ekar
yields the following magnitudes: R(Cousins) = 17.64, V(Johnson) =
17.85; Allington-Smith et al. obtained r = 19.6. On the POSS print
the object is also very faint. It is highly desirable to obtain
complementary UBV photometry, spectroscopy, and polarimetry of this
interesting object during the present high-brightness stage."
1988 March 30 (4573) Daniel W. E. Green
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