On the properties of dust and gas in the environs of V838 Monocerotis

摘要

Aims. We aim to probe the close and distant circumstellar environments of the stellar outburst object V838?Mon. Methods. Herschel far-infrared imaging and spectroscopy were taken at several epochs to probe the central point source and the extended environment of V838?Mon. PACS and SPIRE maps were used to obtain photometry of the dust immediately around V838?Mon, and in the surrounding infrared-bright region. These maps were fitted in 1d and 2d to measure the temperature, mass, and β of the two dust sources. PACS and SPIRE spectra were used to detect emission lines from the extended atmosphere of the star, which were then modelled to study the physical conditions in the emitting material. HIFI spectra were taken to measure the kinematics of the extended atmosphere but unfortunately yielded no detections. Results. Fitting of the far-infrared imaging of V838?Mon reveals 0.5 ? 0.6 M _(⊙) of ≈19 K dust in the environs ( ≈2.7 ?pc) surrounding V838?Mon. The surface-integrated infrared flux (signifying the thermal light echo), and derived dust properties do not vary significantly between the different epochs. We measured the photometry of the point source. As the peak of the SED (Spectral Energy Distribution) lies outside the Herschel spectral range, it is only by incorporating data from other observatories and previous epochs that we can usefully fit the SED; with this we explicitly assume no evolution of the point source between the epochs. We find that warm dust with a temperature ~ 300 ?K distributed over a radius of 150–200?AU. We fit the far-infrared lines of CO arising from the point source, from an extended environment around V838?Mon. Assuming a model of a spherical shell for this gas, we find that the CO appears to arise from two temperature zones: a cold zone ( T _(kin) ≈ 18 ?K) that could be associated with the ISM or possibly with a cold layer in the outermost part of the shell, and a warm ( T _(kin) ≈ 400 ?K) zone that is associated with the extended environment of V838?Mon within a region of radius of ≈210 ?AU. The SiO lines arise from a warm/hot zone. We did not fit the lines of H _(2) O as they are far more dependent on the model assumed.