Spectroscopy of brown dwarf candidates in IC 348 and the determination of its substellar IMF down to planetary masses

TL;DR

This study conducted a comprehensive survey of the IC 348 cluster, discovering new brown dwarfs down to planetary masses, and found that its initial mass function is consistent with a log-normal distribution, showing no variation at the lowest masses.

Contribution

The paper presents the first extensive census of brown dwarfs in IC 348 down to planetary masses, refining the cluster's initial mass function and providing new insights into substellar formation.

Findings

Discovered 16 new cluster members, including 13 brown dwarfs.

Constructed the IMF down to 13 Jupiter masses, fitting a log-normal distribution.

Found no evidence for IMF variation at planetary masses.

Abstract

Context. Brown dwarfs represent a sizable fraction of the stellar content of our Galaxy and populate the transition between the stellar and planetary mass regime. There is however no agreement on the processes responsible for their formation. Aims. We have conducted a large survey of the young, nearby cluster IC 348, to uncover its low-mass brown dwarf population and study the cluster properties in the substellar regime. Methods. Deep optical and near-IR images taken with MegaCam and WIRCam at the Canada-France-Hawaii Telescope (CFHT) were used to select photometric candidate members. A spectroscopic follow-up of a large fraction of the candidates was conducted to assess their youth and membership. Results. We confirmed spectroscopically 16 new members of the IC 348 cluster, including 13 brown dwarfs, contributing significantly to the substellar census of the cluster, where only 30 brown dwarfs were previously known. Five of the new members have a L0 spectral type, the latest-type objects found to date in this cluster. At 3 Myr, evolutionary models estimate these brown dwarfs to have a mass of ~13 Jupiter masses. Combining the new members with previous census of the cluster, we constructed the IMF complete down to 13 Jupiter masses. Conclusions. The IMF of IC 348 is well fitted by a log-normal function, and we do not see evidence for variations of the mass function down to planetary masses when compared to other young clusters.