A&A 458, 191-201 (2006)
DOI: 10.1051/0004-6361:20054641

Triggered massive-star formation on the borders of Galactic H II regions

III. Star formation at the periphery of Sh2-219

L. Deharveng¹, B. Lefloch², F. Massi³, J. Brand⁴, S. Kurtz⁵, A. Zavagno¹ and J. Caplan<sup>1

1</sup>  Laboratoire d'Astrophysique de Marseille, 2 place Le Verrier, 13248 Marseille Cedex 4, France
    e-mail: lise.deharveng@oamp.fr
²  Laboratoire d'Astrophysique de l'Observatoire de Grenoble, 414 rue de la Piscine, BP 53, 38041 Grenoble Cedex 9, France
³  INAF - Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
⁴  INAF - Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy
⁵  Centro de Radioastronomía y Astrofísica, UNAM, Apartado Postal 3-72, 58089 Morelia, Michoacán, México

(Received 5 December 2005 / Accepted 10 July 2006)

Abstract
Context.Massive-star formation triggered by the expansion of H II regions.
Aims.To understand if sequential star formation is taking place at the periphery of the H II region Sh2-219.
Methods.We present ¹²CO  line observations of this region, obtained at the IRAM 30-m telescope (Pico Veleta, Spain).
Results.In the optical, Sh2-219 is spherically symmetric around its exciting star; furthermore it is surrounded along three quarters of its periphery by a ring of atomic hydrogen. This spherical symmetry breaks down at infrared and millimetre wavelengths. A molecular cloud of about 2000 lies at the southwestern border of Sh2-219, in the H I gap. Two molecular condensations, elongated along the ionization front, probably result from the interaction between the expanding H II region and the molecular cloud. In this region of interaction there lies a cluster containing many highly reddened stars, as well as a massive star exciting an ultracompact H II region. More surprisingly, the brightest parts of the molecular cloud form a "chimney", perpendicular to the ionization front. This chimney is closed at its south-west extremity by H walls, thus forming a cavity. The whole structure is 7.5 pc long. A luminous H emission-line star, lying at one end of the chimney near the ionization front, may be responsible for this structure. Confrontation of the observations with models of H II region evolution shows that Sh2-219 is probably 10⁵ yr old. The age and origin of the near-IR cluster observed on the border of Sh2-219 remain unknown.

Key words: stars: formation -- stars: early-type -- ISM: H II regions -- ISM: individual objects: Sh2-219

© ESO 2006

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