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Circular No. 7843 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. IAUSUBS@CFA.HARVARD.EDU or FAX 617-495-7231 (subscriptions) CBAT@CFA.HARVARD.EDU (science) URL http://cfa-www.harvard.edu/iau/cbat.html ISSN 0081-0304 Phone 617-495-7440/7244/7444 (for emergency use only) SAX J1805.5-2031 P. Lowes, National Institute for Space Research, Space Research Organization Netherlands (SRON), Utrecht, and BeppoSAX Science Operation Center (BSOC), Rome; J. J. M. in 't Zand, Astronomical Institute, Utrecht University, and SRON; J. Heise, SRON; M. Cocchi and L. Natalucci, Istituto di Astrofisica Spaziale e Fisica Cosmica, Rome; G. Gennaro and M. Stornelli, BSOC, report that on Mar. 5.5-5.9 UT, Wide Field Camera unit 1 on BeppoSAX detected a new x-ray transient, designated SAX J1805.5-2031 and located at R.A. = 18h05m34s, Decl. = -20o30'.8 (equinox 2000.0; uncertainty 1'.8, 99-percent confidence). The flux was 0.04 Crab units in the range 2-28 keV. No x-ray bursts were detected. C. B. Markwardt, University of Maryland and Goddard Space Flight Center (GSFC); and E. Smith and J. Swank, GSFC, report that the source SAX J1805.5-2031 was observed by the RXTE PCA at 2-10 keV in monitoring scans of the Galactic bulge region around Mar. 2.97 UT (flux 51 +/- 2 mCrab) and in a 3100-s pointed PCA observation starting Mar. 5.84 (flux 36 +/- 1 mCrab). The position of the source in the PCA scans is consistent with the BeppoSAX WFC position (cf. Lowes et al., above). The 2-20-keV spectrum is well fitted with a combination of blackbody (kT = 0.9 keV) emission and a power law (photon index -2.9) for a column density of 4 x 10**22 cm**-2. No strong pulsations of quasiperiodic oscillations are detected; the total fractional r.m.s. variability of the source is 16 percent in the band 0.001-2048 Hz. Additional RXTE observations are planned. COMET C/2002 C1 (IKEYA-ZHANG) B. G. Marsden (cf. MPEC 2002-D36) and S. Nakano have noted the similarity of the orbits of comets C/2002 C1 and C/1661 C1 and that numerical integration of the 2002 orbit backward yields a previous perihelion date within a couple of years of 1659, making the link rather likely. Additional selected visual m_1 estimates: Feb. 14.74 UT, 7.1 (H. Dahle, Copenhagen, Denmark, 9x63 binoculars); 18.95, 6.8 (J. G. de S. Aguiar, Campinas, Brazil, 11x80 binoculars); 20.10, 6.4 (A. Hale, Cloudcroft, NM, 11x80 binoculars); 21.77, 6.3 (A. Kammerer, Ettlingen, Germany, 9x63 binoculars); 24.76, 6.0 (M. V. Zanotta, Laino, Italy, 7x42 binoculars); 28.78, 5.3 (R. J. Bouma, Groningen, The Netherlands, 15x80 binoculars); Mar. 3.75, 4.8 (K. Hornoch, Lelekovice, Czech Republic, naked eye); 4.41, 5.2 (Y. Nagai, Yamanashi, Japan, 12x50 binoculars); 6.49, 5.2 (A. Pearce, Nedlands, W. Australia, 20x80 binoculars). (C) Copyright 2002 CBAT 2002 March 6 (7843) Daniel W. E. Green
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