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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1919
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dc.contributor.authorGhosh, S. K-
dc.contributor.authorMookerjea, B-
dc.date.accessioned2007-10-24T07:40:24Z-
dc.date.available2007-10-24T07:40:24Z-
dc.date.issued1999-
dc.identifier.citationBASI, Vol. 27, No. 1, pp. 151 - 154en
dc.identifier.urihttp://hdl.handle.net/2248/1919-
dc.description.abstractThe diagnostic values of various atomic/ nebular infrared spectral lines of relatively abundant elements (in different ionization states) in Galactic star forming regions, have been studied quantitatively. The code CLOUDY (Ferland 1996)has been used to model spherically symmetric interstellar clouds with embedded ZAMS stars / Young star clusters. In particular, the question of deciphering the upper mass limit of initial mass function has been addressed, in the light of the capabilities of the two spectrometers onboard Infrared Space Observatory (ISO-SWS covering 2.5 - 45 μm; & ISO-LWS covering 45 - 200 μm).en
dc.format.extent261688 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.urihttp://adsabs.harvard.edu/abs/1999BASI...27..151Gen
dc.subjectInfrared Spectral linesen
dc.subjectSpectroscopicen
dc.subjectMass functionen
dc.subjectInfrared space observatory(ISO)en
dc.titleInfrared spectroscopic diagnostics for initial mass functionen
dc.typeArticleen
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