{ "id": "2405.11321", "version": "v1", "published": "2024-05-18T15:31:22.000Z", "updated": "2024-05-18T15:31:22.000Z", "title": "HCN as a probe of the inner disk in a candidate proto-brown dwarf", "authors": [ "B. Riaz", "W. -F. Thi", "M. N. Machida" ], "comment": "Accepted in MNRAS Letters", "categories": [ "astro-ph.SR", "astro-ph.GA" ], "abstract": "The detection of Keplerian rotation is rare among Class 0 protostellar systems. We have investigated the high-density tracer HCN as a probe of the inner disk in a Class 0 proto-brown dwarf candidate. Our ALMA high angular resolution observations show the peak in the HCN (3-2) line emission arises from a compact component near the proto-brown dwarf with a small bar-like structure and a deconvolved size of $\\sim$50 au. Radiative transfer modelling indicates that this HCN feature is tracing the innermost, dense regions in the proto-brown dwarf where a small Keplerian disk is expected to be present. The limited velocity resolution of the observations, however, makes it difficult to confirm the rotational kinematics of this feature. A brightening in the HCN emission towards the core center suggests that HCN can survive in the gas phase in the inner, dense regions of the proto-brown dwarf. In contrast, modelling of the HCO$^{+}$ (3-2) line emission indicates that it originates from the outer pseudo-disk/envelope region and is centrally depleted. HCN line emission can reveal the small-scale structures and can be an efficient observational tool to study the inner disk properties in such faint compact objects where spatially resolving the disk is nearly impossible.", "revisions": [ { "version": "v1", "updated": "2024-05-18T15:31:22.000Z" } ], "analyses": { "keywords": [ "inner disk", "candidate proto-brown dwarf", "line emission", "alma high angular resolution observations", "dense regions" ], "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable" } } }