Dynamical Masses of Young Stellar Multiple Systems with the VLBA (DYNAMO-VLBA)

TL;DR

This study uses VLBA radio interferometry to measure the masses of young stars in multiple systems, revealing discrepancies with theoretical models and providing new dynamical mass estimates for systems in star-forming regions.

Contribution

First VLBA dynamical mass measurements of young stellar systems S1 and EC 95, improving understanding of stellar masses and testing theoretical models.

Findings

S1A has a mass of 4.11 M_sun, less than expected from models.

EC 95A and EC 95B have masses around 2 M_sun, consistent with HR diagram.

Mass of EC 95C estimated at 0.26 M_sun, first such measurement.

Abstract

Very Long Baseline Interferometry (VLBI) provides high angular resolution images and has been used for stellar astrometry for decades. The DYNAMO-VLBA project utilizes the Very Long Baseline Array (VLBA) to study tight binary and multiple pre-main sequence stars, whose components have detectable radio emission and typical separations on the order of milli-arcseconds. Such systems cannot be resolved by Gaia, making VLBI an essential tool for the study of their orbital parameters and, eventually, the determination of their mass. Here, we report VLBA dynamical mass measurements of the individual stars in the S1 system in Ophiuchus and EC\,95 in Serpens. S1 is the most luminous and massive stellar member of the nearby Ophiuchus star-forming region. We find that the primary component, S1A, has a mass of $4.11 \pm 0.10\,M_{\odot}$. This is significantly less than the value of $\sim6\,M_{\odot}$ expected from theoretical models given the location of S1A on the HR diagram. The secondary, S1B, has a mass of $0.831 \pm 0.014\,M_{\odot}$ and is most likely a T Tauri star. In the Serpens triple system EC\,95, we measure the masses of EC\,95A and EC\,95B, finding $2.15\pm0.10$ M$_\odot$ and $2.00\pm0.12$ M$_\odot$, respectively. In this case, the measured masses agree with the location of the stars in the HR diagram for very young 2 $M_\odot$ stars. For the first time, we also estimated the mass of tertiary, EC\,95C, to be 0.26 $^{+0.53}_{-0.46}$ M$_\odot$.