Spectroscopy of Very Low Mass Stars and Brown Dwarfs in the Lambda Orionis Star Forming Region. I. Enlarging the census down to the planetary mass domain in Collinder 69

TL;DR

This study constructs a comprehensive spectroscopic census of Collinder 69, a star-forming region, to understand the formation of brown dwarfs and planetary mass objects by analyzing their spectral features, youth indicators, and spatial distribution.

Contribution

It provides the most complete spectroscopic census of Collinder 69 down to planetary masses, including a new temperature scale and insights into formation mechanisms.

Findings

Confirmed ~90 cluster members spectroscopically.

Assembled a detailed initial mass function from 0.016 to 20 M⊙.

Analyzed spatial distribution to infer formation processes.

Abstract

Whilst there is a generally accepted evolutionary scheme for the formation of low-mass stars, the analogous processes when moving down in mass to the brown dwarfs regime are not yet well understood. In this first paper we try to build the most complete and unbiased spectroscopically confirmed census of the population of Collinder 69, the central cluster of the Lambda Orionis star forming region, as a first step in addressing the question of how brown dwarfs and planetary mass objects form. We have studied age dependent features in optical and near-infrared spectra of candidate members to the cluster (such as alkali lines and accretion associated indicators). In addition, we have complemented that study with the analysis of other youth indicators like X-ray emission or mid-infrared excess. We have confirmed the membership to Collinder 69 of \sim90 photometric candidate members. As a byproduct we have determined a temperature scale for young M, very low-mass stars and brown dwarfs. We have assembled one of the most complete Initial Mass Functions from 0.016 to 20 M\odot. And, finally, we have studied the implications of the spatial distribution of the confirmed members on the proposed mechanisms of brown dwarfs formation.