Central Bureau for Astronomical Telegrams
IAUC 3795: PSR 1937+214; 11 Cam; 3C 273
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Read IAUC 3796
Circular No. 3795
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 617-864-5758
PSR 1937+214
R. N. Manchester, B. A. Peterson and P. T. Wallace report:
"We have detected optical pulses, with the 4-m Anglo-Australian
telescope, at the 0.0016-s period of PSR 1937+214. The pulse
profile has two components separated by ~ 40 percent of the period.
Pulses were detected at the same phase on two successive nights,
Apr. 20 and 21, using a 3".5 aperture centered on a red star (R =
19.4) at R.A. = 19h37m28s78, Decl. = +21deg28'03".3 (equinox 1950.0, FK4
system); this is the candidate star suggested by Djorgovski (1982,
Nature 300, 618). The observed pulse variation is ~ 1 percent of
the star's total light. Our astrometry from a CCD image appears
to place the star 2" north of the VLA radio position (IAUC 3743)
and has a 2-sigma internal error of 0".5: the errors in the primary
reference frame of SAO stars are unknown. The star is considerably
brighter on our CCD image than on the Palomar Sky Survey red
plate. The stellar spectrum exhibited no strong emission lines."
11 CAMELOPARDALIS
L. Pastori, Milano-Merate Observatory, communicates: "
Spectrographic observations (30 A/mm dispersion) of 11 Cam, an extreme
Be star with the first lines of the Balmer series always in
emission, made on 1982 Dec. 13 and 29, show the appearance of the
emission features in the H lines up to H-12. This behavior is
similar to that observed in the outbursts of 1916-19, 1929-31 and
1943-49. Moreover, the Fe II emissions at 454.95 and 458.38 nm
show an increase in intensity and have become clearly discernible,
contrary to previous spectra. This star, then, seems to have
entered a new activity phase."
3C 273
P. A. R. Ade, Queen Mary College, London; I. G. Nolt, University
of Oregon, Eugene; E. I. Robson, Preston Polytechnic, Lancashire;
and M. G. Smith, Royal Observatory, Edinburgh, report: " Recent
millimeter, submillimeter and infrared photometry of 3C 273
shows that this source has flared over the past year. For example,
the 1.1-mm flux density increased from 12 Jy in April 1982 to
22 Jy in early Feb. 1983 and to 37 Jy in early March; the relative
photometric uncertainty is conservatively estimated as less than
10 percent. The observations suggest that the flare may have
propagated from the infrared to successively longer wavelengths."
1983 April 29 (3795) Daniel W. E. Green
Read IAUC 3796
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