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Dust-to-gas ratio and metal abundance in dwarf galaxies
dc.contributor.author | Lisenfeld , Ute | |
dc.contributor.author | Ferrara, A. | |
dc.date.accessioned | 2013-11-07T08:23:52Z | |
dc.date.available | 2013-11-07T08:23:52Z | |
dc.date.issued | 1998 | |
dc.identifier.citation | Lisenfeld, U.; Ferrara, A. Dust-to-gas ratio and metal abundance in dwarf galaxies. Astrophysical Journal, 496(1): 145-154 (1998). [http://hdl.handle.net/10481/29061] | es_ES |
dc.identifier.issn | 0004-637X | |
dc.identifier.issn | 1538-4357 | |
dc.identifier.other | doi: 10.1086/305354 | |
dc.identifier.other | arXiv:astro-ph/9705037v2 | |
dc.identifier.uri | http://hdl.handle.net/10481/29061 | |
dc.description.abstract | We have compared the metallicity (represented by oxygen abundance), and the dust-to-gas ratio, in a sample of dwarf galaxies. For dwarf irregulars (dIrrs) we find a good correlation between the two quantities, with a power-law index 0.54±0.2. Blue Compact Dwarf (BCD) galaxies do not show such a good correlation; in addition both the dust-to-gas ratio and the metallicity tend to be higher than for dIrrs. We have then developed a simple but physical analytical model for the above relation. Comparing the model results with the data, we conclude that: (i) for low values of the dust-to-gas ratio, the relation between the dust-to-gas ratio and the metallicity is quasi-linear, whereas for higher values the curve strongly deviates from the linear behavior, implying that the commonly used power-law approximation is very poor; (ii) the deviation from the linear behavior depends critically on the parameter χ, the ``differential'' mass outflow rate from the galaxy in units of the star formation rate (SFR); (iii) the shape of the curve representing the relation between the dust-to-gas ratio and the metallicity does not depend on the SFR, but only on χ; however, the specific location of a given galaxy on the curve does depend on ψ; (iv) the BCD metallicity segregation is due to a higher ψ, together with a significant differential mass outflow. Thus, the lack of correlation can be produced by largely different star formation rates and values of χ in these objects. | es_ES |
dc.description.sponsorship | U. L. gratefully acknowledges the receipt of a grant by the Deutsche Forschungsgemeinschaft (DFG) and by the Comisi´on Interministerial de Ciencia y Technolog´ıa (Spain). | es_ES |
dc.language.iso | eng | es_ES |
dc.publisher | American Astronomical Society; Institute of Physics (IOP) | es_ES |
dc.rights | Creative Commons Attribution-NonCommercial-NoDerivs 3.0 License | es_ES |
dc.rights.uri | http://creativecommons.org/licenses/by-nc-nd/3.0/ | es_ES |
dc.subject | ISM | es_ES |
dc.subject | Abundances | es_ES |
dc.subject | Dust | es_ES |
dc.subject | Extinction | es_ES |
dc.subject | Galaxies | es_ES |
dc.subject | Irregulars | es_ES |
dc.subject | Evolution | es_ES |
dc.subject | Infrared | es_ES |
dc.title | Dust-to-gas ratio and metal abundance in dwarf galaxies | es_ES |
dc.type | info:eu-repo/semantics/preprint | es_ES |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | es_ES |