FAUST XXIX. OCS line emission: a new method for measuring the luminosity of embedded protostars in binary systems

TL;DR

This paper introduces a novel method using OCS line emission to measure the luminosity of embedded protostars in binary systems, overcoming limitations of traditional dust continuum methods.

Contribution

The paper presents a new observational technique based on OCS molecular lines and quantum calculations to estimate protostellar luminosities in unresolved binary systems.

Findings

Measured luminosities of binary components A1 and A2 are comparable within errors.

Validated the method on NGC1333 IRAS4A using ALMA data.

Discussed the method's reliability and potential applications.

Abstract

The luminosity of embedded protostars is commonly measured via observations of the dust continuum spectral energy distribution from millimetre to infrared wavelengths. However, this method cannot be applied to embedded protostars in binary or multiple systems, where their components are usually unresolved over this extended wavelength range. We propose a new method, based on the idea that a molecule formed (mainly) on the grain surfaces only emits lines in the region where it thermally sublimates from the grain mantles, heated by the photons emitted by the embedded source. In this respect, carbonyl sulfide (OCS) is an optimal molecule, because of its low binding energy and rotational lines in the millimetre. We apply the method to the protobinary system NGC1333 IRAS4A, using ALMA high-spatial resolution ($\sim$50 au) observations of the OCS(19-18) line as part of the ALMA Large Program FAUST. We also present new quantum mechanics calculations of the OCS binding energy distribution, essential for the application of the method. We found that the two binary components, A1 and A2, have a comparable luminosity within the error bars, 7.5$\pm$2.5 and 7$\pm$1 L$_\odot$, respectively. We discuss the reliability of the estimated luminosities and the potential of this new method for measuring the luminosity of embedded protostars in binary and multiple systems.