We observed the “ micro-quasar ” GRS 1758–258 four times with Chandra .
Two HRC-I observations were made in 2000 September-October spanning an intermediate-to-hard spectral transition ( identified with RXTE ) .
Another HRC-I and an ACIS/HETGS observation were made in 2001 March following a hard-to-soft transition to a very low flux state .
The accurate position ( J2000 ) of the X-ray source is RA = 18 01 12.40 , Dec = - 25 44 36.0 ( 90 % confidence radius = 0 ^ { \prime \prime } .6 ) , consistent with the purported variable radio counterpart .
All images are consistent with GRS 1758–258 being a point source , indicating that any bright jet is less than \sim 1 light-month in projected length , assuming a distance of 8.5 kpc .
The March spectrum is well-fit with a multi-color disk-blackbody with an inner temperature of 0.50 \pm 0.01 keV , interstellar absorption of n _ { H } = ( 1.59 \pm 0.05 ) \times 10 ^ { 22 } cm ^ { -2 } , and ( un-absorbed ) 1 - 10 keV luminosity of 4.5 \times 10 ^ { 36 } ( D / 8.5 kpc ) ^ { 2 } ergs s ^ { -1 } .
No narrow emission lines are apparent in the spectrum and upper limits to line equivalent widths are given .