On the history of the interplay between HD 56925and NGC 2359

Free access article

Issue		A&A Volume 366, Number 1, January IV 2001


Page(s)		146 - 156
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20000095

A&A 366, 146-156 (2001)
DOI: 10.1051/0004-6361:20000095

On the history of the interplay between HD 56925and NGC 2359

J. R. Rizzo¹, J. Martín-Pintado¹ and J. G. Mangum²

¹ Observatorio Astronómico Nacional, Aptdo. Correos 1143, 28800 Alcalá de Henares, Spain
² NRAO, 949 N. Cherry Avenue, Tucson, AZ 85721, USA

(Received 20 October 2000 / Accepted 03 November 2000)

Abstract
NGC 2359is an optical nebula excited by the powerful wind and the radiation of the Wolf-Rayet star HD 56925. We have investigated the interaction between this massive star and the surrounding neutral gas by analyzing the large-scale 21 cm-HIemission and by mapping the nebula in the J= $1 \rightarrow 0$ and the J= $2 \rightarrow 1$ lines of CO. We found a conspicuous ( $70 \times 37$ pc) HIshell, expanding at 12 km s^-1, likely produced during the main-sequence phase of the star. The molecular gas towards NGC 2359shows three velocity components. Two of these components, A1 and A2, have narrow linewidths (1-2 km s^-1) and radial velocities of 35-38 and 64-68 km s^-1, respectively. The third component is detected at radial velocities between 50 and 58 km s^-1and has a broader profile (up to 5.5 km s^-1). Furthermore, this component is morphologicaly related with the nebula and has a velocity gradient of a few km s^-1. We have also estimated the physical parameters of the molecular gas by means of a LVG modelling of the CO emission. The gas projected onto the southern HII region of the nebula has low CO column density and is rather hot, probably up to 80 K. Several profiles of the ¹³CO J= $1 \rightarrow 0$ line near the peak of the emission, together with a weak emission bridge between the broad and one of the narrow components (component A2), suggest the presence of a shock front acting in the southern part of the nebula. This shock was likely produced in a previous RSG/LBV phase of HD 56925.

Key words: stars: individual (HD 56925) -- stars: Wolf -- Rayet -- stars: winds -- ISM: bubbles -- ISM: individual (NGC 2359) -- ISM: kinematics and dynamics

Offprint request: J. R. Rizzo

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