We present IR ux density measurements, models of the broadband SED, and results of SED modeling for the Pulsar Wind Nebula (PWN) 3C 58. We nd that the Herschel ux density seems to be slightly lower than suggested by interpolation of previous measurements in nearby wavebands, implying that there may be multiple electron populations in 3C 58. We model the SED using a simple stationary one-zone and a more realistic time-evolving multi-zone scenario. The latter includes variations of ow properties in the PWN (injected energy, magnetic eld, and bulk speed), radiative energy losses, adiabatic expansion, and diusion, similar to previous PWN models. From the modeling, we nd that a PWN age of 2900{5400 yrs is preferred and that there may be excess emission at  1011 Hz. The latter may imply multiple populations of electrons in the PWN.

Abstract
1. INTRODUCTION
2. CHARACTERIZING THE IR SED OF 3C 58
    2.1. Flux Density Measurements
    2.2. IR Slope Constraints
3. MODELING THE BROADBAND SED OF 3C 58
    3.1. One-Zone Model
    3.2. Multi-Zone Model
4. DISCUSSION AND CONCLUSIONS
REFERENCES

• Seungjong Kim(Department of Astronomy and Space Science, Chungbuk National University)
• Jaegeun Park(Department of Astronomy and Space Science, Chungbuk National University)
• Hongjun An(Department of Astronomy and Space Science, Chungbuk National University) Corresponding author