Central Bureau for Astronomical Telegrams
IAUC 5486: 1992a; V590 Mon
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Circular No. 5486
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
COMET HELIN-ALU (1992a)
Ephemeris continuation from the orbital elements on MPC 19818:
1992 TT R. A. (2000) Decl. Delta r Elong. Phase m1
Mar. 29 7 40.72 - 3 02.5 2.732 3.176 107.4 17.5 15.7
Apr. 8 7 43.72 - 3 38.0 2.827 3.147 99.2 18.3 15.7
18 7 48.72 - 4 15.1 2.925 3.120 91.7 18.8 15.8
28 7 55.51 - 4 55.6 3.023 3.095 84.6 18.9 15.8
May 8 8 03.89 - 5 41.1 3.119 3.074 78.1 18.7 15.8
18 8 13.67 - 6 32.9 3.212 3.056 72.1 18.4 15.9
28 8 24.64 - 7 31.9 3.301 3.041 66.4 17.8 15.9
June 7 8 36.66 - 8 38.6 3.384 3.029 61.2 17.1 16.0
17 8 49.57 - 9 53.5 3.461 3.020 56.4 16.3 16.0
27 9 03.24 -11 16.7 3.533 3.015 51.9 15.4 16.0
July 7 9 17.58 -12 48.1 3.599 3.012 47.8 14.5 16.1
17 9 32.50 -14 27.5 3.659 3.013 44.1 13.6 16.1
27 9 47.91 -16 14.3 3.714 3.018 40.7 12.7 16.1
Aug. 6 10 03.76 -18 08.2 3.764 3.025 37.6 11.8 16.2
V590 MONOCEROTIS
M. Perez, Computer Sciences Corporation and IUE Observatory; D.
Geisler, Cerro Tololo Interamerican Observatory; M. Joner, Brigham
Young University; and D. de Winter, European Southern Observatory and
University of Amsterdam, e-mail: "Recent CTIO photometric and ESO
spectroscopic observations of the Herbig Be star V590 Mon = LH alpha 25
= Walker 90 = NGC 2264-62 indicated V = 12.79 +/- 0.01 on Mar. 24.06 UT
and a strong H alpha emission superimposed on a weak continuum showing
no appreciable changes from previous observations. We have been
unable to confirm the claim by Bhatt and Sagar (1992, A.Ap.Suppl. 92,
473) that the object was at V = 9.7. Our previous monitoring over the
years 1988-1991, which includes several observations nearly
contemporaneous with those reported by Bhatt and Sagar, has revealed
variations of smaller than 0.07 mag around V = 12.73 and of 0.02 mag
around V-R = +0.172. We suspect that the published claim is likely to
be a misindentification. Futhermore, IUE observations on Mar. 28.84
and on 28.99 UT with the short- and long-wavelength cameras,
respectively (0.12 to 0.32 nm), revealed only the usual variability in
the various C I, Fe II and Mg II lines."
1992 March 31 (5486) Brian G. Marsden
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