FIR Science Cases

Basically this wavelength range allows a unique probe into objects during their formation as it provides direct access to the peak of the lower temperature black-body emission from the dust which enshrouds them and to a wealth of atomic and molecular spectral lines critical in understanding their energy balance and chemical evolution. 

Separated in four general groups, the science cases the astronomical community is currently more interested in are presented below according to the White Paper submitted in response to the European Space Agency s call for the L2 and L3 L-class missions (Sauvage et al. 2013). 

Most planetary systems are pervaded by dust due to the planet formation process, where through coagulation of dust and gas accretion in the disks that develop during the collapse and infall of massive protostar envelopes planets are formed. By studying the structure and dynamics of this dust, which is very bright at the Far Infrared wavelengths, one can gain information on how such systems were formed. Once the planets are formed, as their motion influence the distribution of the dust, planetary orbits can be traced. 

The emission of organic molecules that could be the building blocks of life in the Universe, such as ammonia and water, can be observed at the FIR region of the spectrum as well. Understanding the contents and chemistry of the Inter Stellar Medium (ISM) can be beneficial to asses the potential for life in these planetary systems. 

Herschel provided unprecedented sensitivity for FIR spectroscopy and improved the angular resolution over ISO, but it was not enough to differentiate spatially the AGN and starburst components. With 0.1-1 arcsecond angular resolution almost all the components of nearby AGNs (Cen A, NGC 1068, Circinus) could be resolved, from the molecular torus (lOpc) out to the outflow and jet structure (Ikpc). 

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