we propose to obtain complete 2.5-45 micron grating spectra with the sws of a sample of dusty m-supergiants. in a recent paper we have shown that some m-supergiants display in their mid-ir spectra not only the expected 9.7 micron silicate feature, but also the family of unidentified infrared bands at 7.7, 8.7, 10.5, 11.3 and 12.7 microns. the uir bands are recognised as diagnostics of regions with carbon-rich chemistries, but from optical spectra and the presence of the silicate dust features m-supergiants are seen to have oxygen- rich chemistries. therefore the appearance of uir bands in m-supergiant spectra is entirely unexpected. we concluded that chromospheres around the m-supergiants provide uv photons which photodissociate co in their stellar winds, yielding free carbon which then builds the polycyclic aromatic hydrocarbons (pahs) responsible for the uir bands. here we will be able to detect the entire family of known uir bands in a sample of m-supergiants having a wide range of mass-loss rates, in 3 ob associations, in order to better determine the conditions under which the uir bands do or do not appear in m-supergiant spectra. by determining which of the known bands appears, we hope to be able to characterise the type and size of pah molecules present around each star.
Instrument
SWS01
Temporal Coverage
1996-07-27T21:25:59Z/1998-01-11T18:53:49Z
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, SKINNER et al., 1999, 'PAHS AND CHROMOSPHERES IN M-SUPERGIANTS', 1.0, European Space Agency, https://doi.org/10.5270/esa-3tg4rl8
