2005A&A...441.1043F

New Canadian Galactic Plane Survey radio continuum, ROSAT X-ray, and optical line observations of supernova remnant (SNR) 3C434.1 (G94.0+1.0) are presented. A radio spectrum of index α=0.4 (where S∝ν^–α) confirms this SNR's emission signature as predominantly synchrotron, and suggests the SNR is in the Sedov expansion phase. The morphology of the remnant is compared in X-ray, optical, and radio continuum, and the brightest emission in all three wavelength regimes is from the eastern hemisphere of 3C434.1, which marks where the SNR shock is interacting with the inside wall of its stellar wind bubble (SWB) home. The system is determined to be 4.5kpc distant, residing in the Perseus Arm Spiral shock. From a deep Hα mosaic of the region, λ656nm Hα line emission is observed that correlates well with radio synchrotron emission and anticorrelates with X-ray emission from the SNR. The origin of this optical emission is likely dense (n_e=40cm^–3) cooling HII from the wall of the SWB, where the SNR shock has penetrated and become radiative (v_s∼100km/s). The X-ray spectrum of this SNR between 0.5 and 2.4keV is well modelled by a single-temperature thermal plasma (T_e=4.5x10⁶K, n_e=0.2cm^–3). The magnetic field of the bright radio synchrotron emission region is found (under the assumption of near equipartition) to be B∼15µG, a factor of 3 compression of the ambient ISM field (5 µG). The westward extension of 3C434.1 is the result of ongoing free expansion of the shock into the lower density interior of the SWB. I use multiwavelength observations to arrive at a unique solution for an interaction model of 3C434.1 with the SWB, from which the age (t=25000yr) and mass ejected in the explosion (M_ej=15.5M_☉) are determined. I also find an initial blast-wave velocity of 1350km/s, typical of type 1b SNe.