Profiles of interstellar cloud filaments. Observational effects in synthetic sub-millimetre observations

TL;DR

This study evaluates how observational uncertainties, noise, and dust property variations affect the measurement of filament profiles in interstellar clouds using synthetic sub-millimetre observations, confirming the robustness of certain parameters.

Contribution

It provides a detailed analysis of observational biases and uncertainties in filament profile measurements from synthetic Herschel-like data, highlighting the effects of noise and resolution.

Findings

Herschel-like noise levels yield accurate filament parameters within a few percent.

Radiative transfer effects have minor impact on filament profile measurements.

Errors increase significantly with distance and noise, affecting parameter constraints.

Abstract

Sub-millimetre observations suggest that the filaments of interstellar clouds have rather uniform widths and can be described with the so-called Plummer profiles. The shapes of the filament profiles are linked to their physical state. Before drawing conclusions on the observed column density profiles, we must evaluate the observational uncertainties. We want to estimate the bias that could result from radiative transfer effects or from variations of submm dust emissivity. We use cloud models obtained with magnetohydrodynamic simulations and carry out radiative transfer calculations to produce maps of sub-millimetre emission. Column densities are estimated based on the synthetic observations. For selected filaments, the estimated profiles are compared to those derived from the original column density. Possible effects from spatial variations of dust properties are examined. With instrumental noise typical of the Herschel observations, the parameters derived for nearby clouds are correct to within a few percent. The radiative transfer effects have only a minor effect on the results. If the signal-to-noise ratio is degraded by a factor of four, the errors become significant and for half of the examined filaments the values cannot be constrained. The errors increase in proportion to the cloud distance. Assuming the resolution of Herschel instruments, the model filaments are barely resolved at a distance of ~400 pc and the errors in the parameters of the Plummer function are several tens of per cent. The Plummer parameters, in particular the power-law exponent p, are sensitive to noise but can be determined with good accuracy using Herschel data. One must be cautious about possible line-of-sight confusion. In our models, a large fraction of the filaments seen in the column density maps are not continuous structures in three dimensions.