Water emission in NGC1333-IRAS4: The physical structure of the envelope

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dc.creatorMaret, S.
dc.creatorCeccarelli, C.
dc.creatorCaux, E.
dc.creatorTielens, A. G. G. M.
dc.creatorCastets, A.
dc.date2002-09-18
dc.date2002-09-25
dc.date.accessioned2026-07-07T02:05:16Z
dc.date.available2026-07-07T02:05:16Z
dc.descriptionWe report ISO-LWS far infrared observations of CO, water and oxygen lines towards the protobinary system IRAS4 in the NGC1333 cloud. We detected several water, OH, CO rotational lines, and two [OI] and [CII] fine structure lines. Given the relatively poor spectral and spatial resolution of these observations, assessing the origin of the observed emission is not straightforward. In this paper, we focus on the water line emission and explore the hypothesis that it originates in the envelopes that surround the two protostars, IRAS4 A and B, thanks to an accurate model. The model reproduces quite well the observed water line fluxes, predicting a density profile, mass accretion rate, central mass, and water abundance profile in agreement with previous works. We hence conclude that the emission from the envelopes is a viable explanation for the observed water emission, although we cannot totally rule out the alternative that the observed water emission originates in the outflow.
dc.identifierhttps://arxiv.org/abs/astro-ph/0209366
dc.identifierhttp://arxiv.org/abs/astro-ph/0209366
dc.identifierAstron.Astrophys. 395 (2002) 573-585
dc.identifierdoi:10.1051/0004-6361:20021334
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/5047
dc.subjectAstrophysics
dc.titleWater emission in NGC1333-IRAS4: The physical structure of the envelope
dc.typetext

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