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IAUC 6678: N Sco 1997; AX J1820.5-1434

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                                                 Circular No. 6678
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
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Phone 617-495-7244/7440/7444 (for emergency use only)


NOVA SCORPII 1997
     M. Cavagna, Sormano, Italy, reports the following precise
position of Liller's possible nova (IAUC 6675), from a CCD image
obtained on June 7.011 UT (0.5-m reflector):  R.A. = 17h54m11s.22,
Decl. = -30o02'53".0 (equinox 2000.0; estimated mag 9).  G. J.
Garradd, Loomberah, N.S.W., reports the following position end
figures, from a CCD image obtained on June 7.511 (0.25-m f/4.1
reflector):  11s.19, 52".9 (mag 9.2).  The Digital Sky Survey shows
no definite object at this location, though a USNO A1.0 star of mag
R = 18.7, B = 19.0 has position end figures 11s.53, 54".3.
     M. Fujii, Okayama; and H. Kawakita, Osaka, Japan, report that
spectroscopic observations (resolution about 1.2 nm; slit size 424"
x 7") on June 7.62 UT show strong, broad H-alpha emission (FWHM
about 3200 km/s; 0.28-m reflector, instrumental resolution about
550 km/s).
     A. C. Gilmore, Mount John University Observatory, reports the
following photometry of Liller's variable star (which is the middle
of three stars of similar brightness that are about 1' apart,
aligned east-west), obtained with the 0.6-m f/16 reflector:  June
7.507 UT, V = 10.48 +/- 0.01, U-B = -0.17 +/- 0.03, B-V = +0.89
+/- 0.02, V-R = +1.31 +/- 0.01, V-I = +1.95 +/- 0.01 (comparison
stars E790 and E782 from Cousins' E region).
     Visual magnitude estimates:  June 7.15 UT, 10.1 (A. Pereira,
Cabo da Roca, Portugal); 7.99, 10.4 (M. Plsek, Lelekovice, Czech
Republic); 7.991, 9.8 (K. Hornoch, Lelekovice, Czech Republic);
8.12, 10.9 (Pereira).


AX J1820.5-1434
     K. Torii, K. Kinugasa, and S. Kitamoto, Osaka University,
report:  "A new x-ray pulsar, AX J1820.5-1434, has been discovered
with ASCA during a galactic-plane survey project on Apr. 9 at R.A.
= 18h20m29s.5, Decl. = -14o34'24" (equinox 2000.0; preliminary
error radius 0'.5).  A coherent pulsation was detected from the
source with an apparent barycentric pulse period of 152.23 +/- 0.05
s.  The mean flux, not corrected for interstellar absorption, was
2.4 x 10E-11 erg cmE-2 sE-1 in the energy range 1-10 keV.  The
1-10-keV pulse shape has one broad peak with a phase width of 0.3.
At the peak, the pulsed flux is comparable with the flux of the
constant component.  The energy spectra obtained by both the GIS
and the SIS were fitted by a power-law model (photon index of 1.0
+/- 0.4) with a high column density of (1.0 +/- 0.3) x 10E23 H
atoms cmE-2."

                      (C) Copyright 1997 CBAT
1997 June 9                    (6678)            Daniel W. E. Green

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