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tokens: of . The magnetic field strength B and fitted values translate to a radiative lifetime of ∼100 years, which is difficult to explain without distributed in situ acceleration—this requirement can be relaxed by using a lower value of B . Figure 9. Representative models for the SED of the high-energy synchrotron component along with our binned X-ray data for K61 (top) and the NHS (bottom). Dashed vertical lines represent the boundaries of the energy range that NuSTAR is capable of observing. Varying several of the input parameters can have a large effect on the shape of the curve above 7 keV for K61 and especially in the case of the NHS. The bottom of Figure 9 shows several representative models for the SED of the NHS near the NuSTAR energy band. Unlike K61, the low-energy tail of the second emission component of the NHS is not constrained by the radio or near-IR data. The models shown here vary wildly in emission above 7 keV, where the magnetic field strengths ranges over G, with , and , with a comoving luminosity of . Future observations using NuSTAR would allow us to constrain the SED up to ∼ 80 keV. If the X-ray emission is due only to EC/CMB, then an estimate of the magnetic field strength can be made using (Felten Morrison 1966 ), where is the apparent energy density of the CMB at redshift z , erg cm −3 is the local CMB energy density, the apparent temperature of the CMB is , and the temperature of the CMB is . This calculation gives a value of G. While this is comparable to that quoted for other jets where the EC/CMB model is used to model their X-ray emission, in this case a comoving luminosity of is required to fit the model to our X-ray data. We feel this is unrealistic, as it would violate the Eddington limit by many orders of magnitude. For that reason, we have not shown it in any figure. Additionally, assuming an equipartition magnetic field, a Doppler factor of is required for EC/CMB to explain the observed X-ray/radio NHS flux even for the case of using standard formulae (Harris Krawczynski 2002 ). The required beaming is highly unlikely given the observed properties of the 3C 111 jet, e.g., the observed brightness of the SHS and the lack of obvious blazar properties. We do not have many data points with which to constrain the model of the low-energy synchrotron component, especially in K30 and K61. We expect to be able model its SED well in a follow-up paper using JVLA observations of the jet. As well, additional HST and Chandra observations would help to better constrain the near-IR to optical and X-ray spectral indices of the components, and perhaps also constrain the X-ray emission mechanism of additional components. 5. CONCLUSIONS We have presented new Chandra and HST observations of 3C 111 that reveal that its jet has eight X-ray and near-IR/optical emitting components, which extend for 121 arcsec (355 kpc deprojected length) from its AGN nucleus in the approaching jet, and also reveal the hotspot emission on the