CH abundance gradient in TMC-1^⋆

¹ Department of Physics, PO Box 64, 00014 University of Helsinki, Finland
e-mail: aleksi.suutarinen@gmail.com
² Department of Physics, AlbaNova, 10691 Stockholm, Sweden
³ Observatory, University of Helsinki, Finland
⁴ Onsala Space Observatory, 43992 Onsala, Sweden
⁵ GRS mbH, 50667 Cologne, Germany
⁶ Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, University Road, Belfast, BT7 1NN, UK
⁷ Joint Astronomy Centre, Hilo, 96720, USA

Received: 5 November 2010
Accepted: 14 May 2011

Abstract

Aims. The aim of this study is to examine if the well-known chemical gradient in TMC-1 is reflected in the amount of rudimentary forms of carbon available in the gas-phase. As a tracer we use the CH radical which is supposed to be well correlated with carbon atoms and simple hydrocarbon ions.

Methods. We observed the 9-cm Λ-doubling lines of CH along the dense filament of TMC-1. The CH column densities were compared with the total H₂ column densities derived using the 2MASS NIR data and previously published SCUBA maps and with OH column densities derived using previous observations with Effelsberg. We also modelled the chemical evolution of TMC-1 adopting physical conditions typical of dark clouds using the UMIST Database for Astrochemistry gas-phase reaction network to aid the interpretation of the observed OH/CH abundance ratios.

Results. The CH column density has a clear peak in the vicinity of the cyanopolyyne maximum of TMC-1. The fractional CH abundance relative to H₂ increases steadily from the northwestern end of the filament where it lies around 1.0 × 10^-8, to the southeast where it reaches a value of    2.0 × 10^-8. The OH and CH column densities are well correlated, and we obtained OH/CH abundance ratios of  ~16–20. These values are clearly larger than what has been measured recently in diffuse interstellar gas and is likely to be related to C to CO conversion at higher densities. The good correlation between CH and OH can be explained by similar production and destruction pathways. We suggest that the observed CH and OH abundance gradients are mainly due to enhanced abundances in a low-density envelope which becomes more prominent in the southeastern part and seems to continue beyond the dense filament.

Conclusions. An extensive envelope probably signifies an early stage of dynamical evolution, and conforms with the detection of a large CH abundance in the southeastern part of the cloud. The implied presence of other simple forms of carbon in the gas phase provides a natural explanation for the observation of “early-type” molecules in this region.