We have obtained a moderately long ( 10 ^ { 5 } second ) ASCA observation of the Seyfert 1 galaxy Markarian 231 , the most luminous of the local ultraluminous infrared galaxy ( ULIRG ) population .
In the best-fitting model we do not see the X-ray source directly ; the spectrum consists of a scattered power-law component and a reflection component , both of which have been absorbed by a column N _ { H } \approx 3 \times 10 ^ { 22 } { \ > { cm } ^ { -2 } } .
About 3 / 4 of the observed hard X-rays arise from the scattered component , reducing the equivalent width of the iron K \alpha line .
The implied ratio of 1 - 10 keV X-ray luminosity to bolometric luminosity , { L _ { x } } / { L _ { bol } } \sim 2 \% , is typical of Sy 1 galaxies and radio-quiet QSOs of comparable bolometric luminosities , and indicates that the bolometric luminosity is dominated by the AGN .
Our estimate of the X-ray luminosity also moves Mrk 231 in line with the correlations found for AGN with extremely strong Fe II emission .
A second source separated by about 2 arcminutes is also clearly detected , and contributes about 25 \% of the total flux .