Physical parameters of young M-type stars and brown dwarfs with VOSA

TL;DR

This paper demonstrates how the Virtual Observatory SED Analyzer (VOSA) can be effectively used to analyze the physical parameters of young M-type stars and brown dwarfs, leveraging large survey datasets.

Contribution

It introduces the application of VOSA to study a large sample of M-type stars and brown dwarfs, highlighting its capabilities in handling extensive survey data for stellar characterization.

Findings

VOSA successfully derived physical parameters for numerous M-type stars.

The study provided insights into the properties of young M stars and brown dwarfs.

The approach enhances the efficiency of analyzing large stellar samples.

Abstract

Although M dwarfs are the most common stars in our stellar neighborhood they are still among the least understood. This class of objects is dominated by dramatic changes: in their interiors (fully convective, with implications in angular momentum evolution), in their atmospheres (crossing temperatures where dust settling occurs), and in their nature (including both, stellar and substellar objects). Populating efficiently our solar neighborhood, they are very well represented in the databases coming from new and more sensitive surveys that provide photometry at many wavelength ranges and cover large areas of the sky (few examples among many others are GALEX, SDSS, 2MASS, WISE and VISTA). In this context of opulence of objects and data, the Virtual Observatory comes in naturally as an excellent framework to efficiently advance in the knowledge of M-type sources. We put special emphasis in the benefits of using the new capabilities of VOSA (Virtual Observatory SED Analyzer, Bayo et al. 2008; in operation since 2008 and in constant development) to study large samples of candidate and confirmed M members of Chamaeleon I.