Dust scattering from the taurus molecular cloud

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7124

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DC Field	Value	Language
dc.contributor.author	Sathya Narayan	-
dc.contributor.author	Murthy, J	-
dc.contributor.author	Narayanankutty, K	-
dc.date.accessioned	2020-11-17T14:11:29Z	-
dc.date.available	2020-11-17T14:11:29Z	-
dc.date.issued	2017-04	-
dc.identifier.citation	Monthly Notices of the Royal Astronomical Society, Vol. 466, No. 3, pp. 3199-3205	en_US
dc.identifier.issn	1365-2966	-
dc.identifier.uri	http://prints.iiap.res.in/handle/2248/7124	-
dc.description	Restricted Access © Royal Astronomical Society https://doi.org/10.1093/mnras/stw3280	en_US
dc.description.abstract	We present an analysis of the diffuse ultraviolet emission near the Taurus Molecular Cloud based on observations made by the Galaxy Evolution Explorer. We used a Monte Carlo dust scattering model to show that about half of the scattered flux originates in the molecular cloud with 25 per cent arising in the foreground and 25 per cent behind the cloud. The best-fitting albedo of the dust grains is 0.3, but the geometry is such that we could not constrain the phase function asymmetry factor (g).	en_US
dc.language.iso	en	en_US
dc.publisher	Oxford University Press on behalf of the Royal Astronomical Society	en_US
dc.subject	Ultraviolet: ISM	en_US
dc.title	Dust scattering from the taurus molecular cloud	en_US
dc.type	Article	en_US
Appears in Collections:	IIAP Publications

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