in the data taken with isocam-cvf around the exciting source of the trifid nebula (proposals com_glo and trifid) we have found warm dust around the star (see figure 1 and 2). other stars in the trifid also show the same behaviour. this result is very important for the study of massive star formation and induced star formation. it means that the central object of trifid is extremely young as it has not been able to dissipate all the material around it. the star is of o7 v type and has ionized one important fraction of the gas around it. however, a dust envelope has survived to the strong uv field. the stellar spectrum shows the silicate feature in emission. around the star this feature is detected at several positions, but shifted towards longer wavelengths. probably the dust solid state features at different locations are excited under different physical conditions. the dust continuum emission increases dramatically around the star (the spectrum is different from the stellar one what means that there is not contamination from the central object). the unprecedent informations provided by the proposed observations, together with our on-going studies of the molecular content, and our detailed chemical and hydrodynamical modelling, will lead to a complete picture of the trifid nebula and will supply a full description of the physical and chemical properties of the interstellar dust.
Instrument
CAM01 , CAM04
Temporal Coverage
1997-06-16T00:22:26Z/1998-04-11T11:00:52Z
Version
1.0
Mission Description
The Infrared Space Observatory (ISO) was the worlds first true orbiting infrared observatory. Equipped with four highly-sophisticated and versatile scientific instruments, it was launched by Ariane in November 1995 and provided astronomers world-wide with a facility of unprecedented sensitivity and capabilities for a detailed exploration of the Universe at infrared wavelengths.
European Space Agency, CERNICHARO et al., 2024, 'WARM DUST AROUND HOT STARS : THE IONIZING SOURCE OF THE TRIFID NEB', 1.0, European Space Agency, https://doi.org/10.5270/esa-luhkqds
