supernovae have been considered to be one of the major energy source for the interstellar space, and a significant part of the energy is probably supplied through dynamical processes, such as the interstellar shock propagating in the gas clouds. however, the amount of the dynamical energy transfer from supernovae to the interstellar gas has not been known. recent theoretical work reveals that the oi 63 micron line emission is the dominant cooling process of the shocked gas. therefore, we can evaluate the dynamically transfered energy from the supernova to the interstellar gas from the total luminosity of the oi 63 line emission. on the other hand, the infrared telescope in space (irts) launched in early 1995 has the far-infrared line mapper (film, shibai et al 1994), which will make a mapping of the oi line intensity with a 8 x 13 arcmin beam. the film on the irts can make a mapping of about 10 % of the sky that includes several prominent supernova remnants, such as ic443, rcw86, and g117.4+5.0. these snr.s have a large shell larger than 30 arcmin. this proposal is to make a complementary observation with the film/irts. the lws has a wider spectral coverrage and a finer spatial resolution. therefore, only from both of the lws/iso and film/irts, we can obtain an accurate evaluation for the dynamical energy transfer from the supernovae to the interstellar gas.
Instrument
LWS01
Temporal Coverage
1996-04-04T03:58:37Z/1996-04-04T07:41:39Z
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, NAKAGAWA et al., 1999, 'IRTS FOLLOW-ON OBSERVATION OF SNR.S WITH FIR FINE STRUCTURE LINES', 1.0, European Space Agency, https://doi.org/10.5270/esa-13kku0p
