Detection of CH3+ in the O-rich planetary nebula NGC 6302
Charmi Bhatt, Jan Cami, Els Peeters, Nicholas Clark, Paula Moraga Baez, Kevin Volk, G. C. Sloan, Joel H. Kastner, Harriet L. Dinerstein, Mikako Matsuura, Bruce Balick, Kathleen E. Kraemer, Kay Justtanont, Olivia Jones, Raghvendra Sahai, Isabel Aleman, Michael J. Barlow, Jeronimo Bernard-Salas, Joris Blommaert, Naomi Hirano, Patrick Kavanagh, Francisca Kemper, Eric Lagadec, J. Martin Laming, Frank Molster, Hektor Monteiro, Anita M. S. Richards, N. C. Sterling, Maryam Torki, Peter A. M. van Hoof, Jeremy R. Walsh, L. B. F. M. Waters, Roger Wesson, Finnbar Wilson, Nicholas J. Wright, Albert A. Zijlstra
公開日: 2025/9/18
Abstract
Planetary nebulae are sites where ejected stellar material evolves into complex molecules, but the precise physical conditions and chemical routes that govern these processes are unclear. The presence of abundant carbon-rich molecules in O-rich environments poses particular challenges. Here we report the first detection of methyl cation (CH3+) in any planetary nebula, observed in the O-rich nebula NGC 6302 using JWST MIRI/MRS observations. CH3+ is a key driver of organic chemistry in UV-irradiated environments. Spatially resolved observations reveal that CH3+ is co-located with 12CO, H2, H II, HCO+, and Polycyclic aromatic hydrocarbons (PAHs). LTE modelling of the CH3+ emission yields excitation temperatures of 500-800K in the inner bubble and torus, rising to 1000-2000K in the outer bubble of NGC 6302, with column densities ranging from ~10^11 to 10^13 cm^-2. This detection demonstrates that hydrocarbon radical chemistry must be incorporated into planetary nebulae chemical models. Further near-IR observations are crucial to map different chemical networks operating in these environments.