We present a model for the accretion flow around the supermassive black hole in the LINER nucleus of NGC 1097 which fits the optical to X-ray spectral energy distribution ( SED ) .
The X-ray segment of the SED is based on observations with the Chandra X-Ray Observatory , which are reported here for the first time .
The inner part of the flow is modeled as a radiatively inefficient accretion flow ( RIAF ) and the outer part as a standard thin disk .
The value of the transition radius ( r _ { tr } \approx 225 R _ { S } , where R _ { S } = 2 GM / c ^ { 2 } ) between the RIAF and outer thin disk was obtained from our previous fitting of the double-peaked Balmer emission line profile , which originates in the thin disk .
The black hole mass was inferred from measurements of the stellar velocity dispersion in the host galaxy .
When these parameters are used in the accretion flow model , the SED can be successfully reproduced , which shows that the line profile model and the accretion flow model are consistent with each other .
A small remaining excess in the near-UV is accounted by the contribution of an obscured starburst located within 9 pc from the nucleus , as we reported in an earlier paper .
The radio flux is consistent with synchrotron emission of a relativistic jet modeled by means of the internal shock scenario .
In an appendix we also analyze the Chandra X-ray observations of the \sim 1 kpc circumnuclear star-forming ring and of an ultraluminous compact X-ray source located outside the ring .