The relationship between the prestellar core mass function and the stellar initial mass function

TL;DR

This paper investigates how the core mass function influences the stellar initial mass function, finding that a model where all stars form as multiples better explains observed data.

Contribution

It introduces and tests two star formation scenarios, demonstrating that the multiple formation model aligns more closely with observed IMFs.

Findings

Multiple star formation model fits the IMF better

Log-normal CMF is consistent with observations

Binary and triple systems are key to IMF formation

Abstract

Stars form from dense molecular cores, and the mass function of these cores (the CMF) is often found to be similar to the form of the stellar initial mass function (IMF). This suggests that the form of the IMF is the result of the form of the CMF. However, most stars are thought to form in binary and multiple systems, therefore the relationship between the IMF and the CMF cannot be trivial. We test two star formation scenarios - one in which all stars form as binary or triple systems, and one in which low-mass stars form in a predominantly single mode. We show that from a log-normal CMF, similar to those observed, and expected on theoretical grounds, the model in which all stars form as multiples gives a better fit to the IMF.