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Astron. Astrophys. 336, 1024-1028 (1998)

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Thermal dust imaging of the cometary HII region NGC 6334 F *

Paolo Persi 1, Mauricio Tapia 2, Marcello Felli 3, Pierre Olivier Lagage 4 and Marco Ferrari-Toniolo 1

1 Istituto Astrofisica Spaziale, Area di Ricerca Roma-Tor Vergata, Via del Fosso del Cavaliere, I-00133 Roma, Italy
2 Instituto de Astronomia, UNAM, Apartado Postal 877, Ensenada, 22830, B.C., Mexico
3 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze, Italy
4 CEA/DSM/DAPNIA/, Service d'Astrophysique (URA 2052 du CNRS), CE Saclay, F-91191 Gif-sur-Yvette, France

Received 15 April 1998 / Accepted 20 May 1998


Sub-arcsec images at 3.8 and 11.2µm of the cometary HII region NGC 6334 F are presented. Only the HII region is detected at 3.8µm, while three distinct small diameter sources and a diffuse extended emission are found at 11.2µm. The brightest of the small diameter sources (called MIR 2) is coincident with the HII region. MIR 2 is resolved and shows a cometary shape similar to that observed in the radio continuum. This suggests that warm dust and ionized gas are well mixed in the HII region. The diffuse extended emission is observed in the region where the highest density molecular gas and the central region of the molecular outflow are located. No emission at either wavelength is detected from IRS-I 2, the proposed alternative powering source of the bipolar molecular outflow.

Key words: ISM: HII regions – ISM: individual objects: NGC 6334 F – ISM: jets and outflows – infrared: stars

* Based on observations obtained at CFHT and UKIRT on Maona Kea.

Send offprint requests to: P. Persi, (persi@saturn.ias.rm.cnr.it)

© European Southern Observatory (ESO) 1998

Online publication: July 27, 1998