Profile fitting by marquardt algorithm

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5096

Full metadata record

DC Field	Value	Language
dc.contributor.author	Surendiranath, R	-
dc.date.accessioned	2010-04-09T14:25:59Z	-
dc.date.available	2010-04-09T14:25:59Z	-
dc.date.issued	1988	-
dc.identifier.citation	Velusamy, T and Venugopal, V. R eds., Image processing in astronomy: Proceedings of the workshop in imaging processing in astronomy held in Ooty 23 - 27 March 1987, pp. 87 - 89	en
dc.identifier.uri	http://hdl.handle.net/2248/5096	-
dc.description	Open Access	en
dc.description.abstract	Many of the stellar and nebular spectroscopic problems need the inputs of the line flux (or equivalent width if the line is in absorption) and the wavelength of the line peak. These input parameters are then used in the analysis for obtaining physical parameters like electron temperature, electron density, abundances of the elements, radial velocities etc.	en
dc.language.iso	en	en
dc.publisher	Tata Institute of Fundamental Research	en
dc.rights	© Tata Institute of Fundamental Research	en
dc.subject	Marquardt Algorithm	en
dc.subject	Stellar	en
dc.subject	Nebular Spectroscopic	en
dc.subject	Line Flux	en
dc.subject	Electron Temperature	en
dc.subject	Electron Density	en
dc.subject	Radial Velocities	en
dc.title	Profile fitting by marquardt algorithm	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

Files in This Item:

File	Description	Size	Format
Profile fitting by marquardt algorithm		65.58 kB	Adobe PDF	View/Open

DSpace JSPUI