演講資訊

摘要：

We present a detailed analysis of molecular gas in jet-interacting regions of NGC 1068 using ALMA archival data of CO(1-0) and CO(2-1) transitions. We identified a distinct feature where CO(1-0) shows redshifted absorption while CO(2-1) exhibits emission at the same location and velocity observed consistently across several regions along the jet. Spectral profiles of CO(201) reveal redshifted secondary emission components, while CO(0-1) shows blended inverse P-Cygni-like absorption, particularly on the northeast (approaching) side of the jet. These redshifted features are interpreted as inflowing molecular gas, with the CO(201)—only component at ~1230 km s^-1 likely tracing denser of shock-heated gas and CO(1-0) is likely tracing low density clouds or diffuse gas. Our results provide strong evidence for jet-driven inflow, highlighting the dual role of AGN jets in both removing and funneling gas toward the nucleus. Excitation temperatures and optical depths were derived from a combination of emission and absorption line, revealing the physical condition of the gas. Excitation temperatures were derived assuming local thermodynamic equilibrium (LTE), yielding values ranging from 69 K to 83 K across the studied regions. Using optical depth measurements we computer CO column densities (2.61-4.38)*10¹⁴ cm^-2, corresponding to H2 column density of (3.26-5.47) *1014 cm^-2. Molecular gas masses were estimated from the integrated CO(1-0) fluxes, yielding values between 1.85*10⁷ and 2.11*10⁷ solar mass.