Statistical properties and correlation length in star-forming molecular clouds: I. Formalism and application to observations

TL;DR

This paper develops a statistical framework using ergodic theory to analyze density fluctuations in star-forming molecular clouds, addressing biases and uncertainties in observational and simulation data.

Contribution

It introduces a rigorous method to evaluate correlation lengths and statistical errors in molecular cloud data, improving analysis of star formation processes.

Findings

Correlation length is about 1% of cloud size in Polaris and Orion B.

Biases from line-of-sight integration affect density fluctuation statistics.

Statistical errors increase with density contrast, impacting PDF analysis.

Abstract

The proper characterization of the general statistical behavior of these fluctuations, from a limited sample of observations or simulations, is of prime importance to understand the process of star formation. In this article, we use the ergodic theory for any random field of fluctuations, as commonly used in statistical physics, to derive rigorous statistical results. We outline how to evaluate the autocovariance function (ACF) and the characteristic correlation length of these fluctuations. We then apply this statistical approach to astrophysical systems characterized by a field of density fluctuations, notably star-forming clouds. When it is difficult to determine the correlation length from the empirical ACF, we show alternative ways to estimate the correlation length. We show that the statistics of the column-density field is hampered by biases introduced by integration effects along the line of sight and we explain how to reduce these biases. The statistics of the probability density function (PDF) ergodic estimator also yields the derivation of the proper statistical error bars. We provide a method that can be used by observers and numerical simulation specialists to determine the latter. We show that they (i) cannot be derived from simple Poisson statistics and (ii) become increasingly large for increasing density contrasts, severely hampering the accuracy of the low and high end part of the PDF because of a sample size that is too small. As templates of various stages of star formation in MCs, we then examine the case of the Polaris and Orion B clouds in detail. We calculate, from the observations, the ACF and the correlation length in these clouds and show that the latter is on the order of $\sim$1\% of the size of the cloud.