Far Infrared Spectroscopy of star-forming galaxies: Expectations for the Herschel Space Observatory

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dc.creatorMalhotra, Sangeeta
dc.date2001-04-11
dc.date.accessioned2026-07-07T01:58:12Z
dc.date.available2026-07-07T01:58:12Z
dc.descriptionISO has enabled far-infrared spectroscopy of a variety of galaxies. Using the [CII] (158 micron) and [OI](63 micron) lines, we can characterize the physical conditions in the star-forming ISM. These observations also form the basis of our expectations for what the Herschel Space Observatory will observe for high redshift galaxies. While [CII] is suppressed in ULIRGs and normal galaxies with high dust temperatures, it is stronger than expected in metal poor galaxies by factors of a few. Young galaxies at high redshifts might be expected to be both metal poor and actively star-forming, leading to contrary expectations for the [CII] line strength. The best prediction for [CII] detection is derived by using the observed proportionality between [CII] and mid-IR emission from PAHs. Using the observed [CII]/7 micron ratio and number counts from ISO deep surveys we predict that HSO will be able to detect 100 sources/square-degree in the [CII] line.
dc.description4 Pages, uses toledoStyle.cls, to appear in `The Promise of FIRST', ESA SP-460, eds. G.L. Pilbratt et al
dc.identifierhttps://arxiv.org/abs/astro-ph/0104198
dc.identifierhttp://arxiv.org/abs/astro-ph/0104198
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2677
dc.subjectAstrophysics
dc.titleFar Infrared Spectroscopy of star-forming galaxies: Expectations for the Herschel Space Observatory
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