In this article , models are constructed of the compact jet in GRS 1915+105 during an epoch of optimal data capture .
On April 02 , 2003 , the object was observed in the hard X-ray/soft gamma ray band ( INTEGRAL ) , hard X-ray band ( RXTE ) , near IR ( ESO/New Technology Telescope ) and the VLBA ( 8.3 GHz and 15 GHz ) .
The source was in a so-called ” high plateau state. ” The large radio flux provides high signal to noise ratios in the radio images .
Thus , one can image the jet out to large distances ( > 10 ^ { 15 } cm ) .
This combined with the broadband coverage make this epoch the best suited for modeling the jet .
The parametric method developed in the papers ( 11 ; 12 ; 13 ; 37 ) that has been successfully utilized in the realm of extragalactic radio jets is implemented .
The basic model is one where external inverse Compton ( EIC ) scattering of accretion disk photons by jet plasma provides the hard X-ray powerlaw .
Unlike AGN jets , it is found that the radio jet must be highly stratified in the transverse direction in order to produce the observed surface brightness distribution in the radio images .
Various jet models are considered .
The jet power is Q \approx 3 - 4 \times 10 ^ { 38 } ergs/sec if the hard X-ray powerlaw luminosity is from EIC in the jet and Q \approx 2 - 9 \times 10 ^ { 37 } ergs/sec if the X-rays are emitted from the accretion disk corona .
These estimates indicate that the jet power can be as high as 60 % of the total X-ray luminosity .