\title{A New Eclipsing X-Ray Burster near the Galactic Center:
   A Quiescent State of the Old Transient A1742-289 }

\author{Yoshitomo {\sc Maeda}, Katsuji {\sc Koyama}, Masaaki {\sc Sakano}\\
{\it Department of Physics, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto,  606-01 Japan}\\
{\it E-mail (YM) maeda@cr.scphys.kyoto-u.ac.jp} \\
Toshiaki {\sc Takeshima}\\
{\it Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt,MD 20771}\\
and\\
Shigeo {\sc Yamauchi}\\
{\it Faculty of Humanities and Social Sciences, Iwate University, 3-18-34, Ueda, Morioka, Iwate 020}\\
}

\abst{
 With ASCA, we found highly absorbed X-rays from the position of the
bright transient source A1742-289, with variable flux ranging from
8$\times$10$^{-12}$ to 4$\times$10$^{-11}$ erg s$^{-1}$cm$^{-2}$ in
the 3-10 keV band.  We discovered an X-ray burst and eclipses from
A1742-289, establishing that A1742-289 is an eclipsing low mass X-ray
binary.  Using the black body radius during the X-ray burst, we
estimated the distance of A1742-289 to be about 10 kpc, or near the
Galactic Center. Then the burst peak flux was found below the
Eddington limit of a neutron star.  Excess soft X-rays during the
eclipse were detected, which are interpreted to be a scattering by
interstellar dust-grains.  Since A1742-289 was found to be an X-ray
emitter even in the quiescent state with a moderate but variable flux,
and since A1742-289 is lying only 1.3' from the Galactic center,
previously reported X-ray fluxes of the Galactic center (Sgr A*) with
non-imaging instruments might have been suffered by possible
contamination of A1742-289.  }
\kword{ISM: individual(Sagittarius A*) -- Stars:individual(A1742-289) -- Stars:eclipsing -- X-rays:binaries -- X-rays:bursts}



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