Modeling CO Line Profiles in Shocks of W28 and IC44

• DOI: 10.48550/arxiv.2112.03349
• Publication Date: 2021-01-01
• Authors: Nguyen Fuda; Le-Ngoc Tram; W. T. Reach
• Keywords: Line (geometry)

Molecular emission arising from the interactions of supernova remnant (SNR) shock waves and molecular clouds provide a tool for studying dispersion compression that might kick-start star formation as well understanding cosmic ray enhancement in SNRs. Purely-rotational CO created by magneto-hydrodynamic SNR - cloud interaction is an effective tracer, particularly slow-moving, continuous shocks into cold inner clumps cloud. In this work, we present new theoretical radiative transfer framework predicting line profile with Paris-Durham 1D model. We generated predictions produced slow, magnetized C-shocks gas density ~ 100,000 cm-3 speeds 35 50 km s-1. The numerical to reproduce utilizes Large Velocity Gradient (LVG) approximation omission optically-thick plane-parallel slabs. With framework, various spectroscopic observations up J=16 SNRs W28 IC443, obtained SOFIA, IRAM-30m, APEX, KPNO. found prediction offers constraints on velocity preshock independent absolute brightness requiring fewer lines than diagnostics using rotational excitation diagram.