# Fullerenes in the IC 348 star cluster of the Perseus Molecular Cloud

## TL;DR

This study reports the detection of fullerenes C60 and C70 in the star-forming region IC 348, revealing their widespread presence and potential role in organic molecule formation during planet formation.

## Contribution

First detection of fullerenes in the IC 348 star cluster, showing their distribution and possible ionization states in a star-forming environment.

## Key findings

- Fullerenes detected in multiple stars and interstellar locations within IC 348.
- Ionized fullerene species suggest significant ionization fractions.
- Fullerene abundance could account for 0.1% of carbon in protoplanetary disks.

## Abstract

We present the detection of fullerenes C60 and C70 in the star-forming region IC 348 of the Perseus molecular cloud. Mid-IR vibrational transitions of C60 and C70 in emission are found in Spitzer IRS spectra of individual stars (LRLL 1, 2, 58), in the averaged spectrum of three other cluster stars (LRLL 21, 31 and 67) and in spectra obtained at four interstellar locations distributed across the IC 348 region. Fullerene bands appear widely distributed in this region with higher strength in the lines-of-sight of stars at the core of the cluster. Emission features consistent with three most intense bands of the C_{60}^+ and with one of C_{60}^- are also found in several spectra, and if ascribed to these ionized species it would imply ionization fractions at 20 and 10 %, respectively. The stars under consideration host protoplanetary disks, however the spatial resolution of the spectra is not sufficient to disentangle the presence of fullerenes in them. If fullerene abundances in the cloud were representative of IC 348 protoplanetary disks, C60, the most abundant of the two species, could host 0.1 % of the total available carbon in the disks. This should encourage dedicated searches in young disks with upcoming facilities as JWST. Fullerenes provide a reservoir of pentagonal and hexagonal carbon rings which could be important as building blocks of prebiotic molecules. Accretion of these robust molecules in early phases of planet formation may contribute to the formation of complex organic molecules in young planets.