FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3197206788> ?p ?o ?g. }

• W3197206788 endingPage "2765" @default.
• W3197206788 startingPage "2755" @default.
• W3197206788 abstract "ABSTRACT Dust has been detected in high-redshift (z &gt; 5) galaxies but its origin is still being debated. Dust production in high-redshift galaxies could be dominated by stellar production or by accretion (dust growth) in the interstellar medium. Previous studies have shown that these two dust sources predict different grain-size distributions, which lead to significantly different extinction curves. In this paper, by performing radiative transfer calculations, we investigate how the difference in the extinction curves affects the dust attenuation properties of galaxies. To examine the major effects of the dust–stars distribution geometry, we adopt two representative cases in spherical symmetry: the well-mixed geometry (stars and dust are homogeneously mixed) and the two-layer geometry (young stars are more concentrated in the centre). In both cases, we confirm that the attenuation curve can be drastically steepened by scattering and by different optical depths between young and old stellar populations, and can be flattened by the existence of unobscured stellar populations. We can reproduce similar attenuation curves even with very different extinction curves. Thus, we conclude that it is difficult to distinguish dust sources only with attenuation curves. However, if we include information on dust emission and plot the relation between infrared excess (IRX) and the ultraviolet spectral slope (β), then different dust sources predict different positions in the IRX–β diagram. A larger β is preferred under a similar IRX if dust growth is the dominant dust source." @default.
• W3197206788 created "2021-09-13" @default.
• W3197206788 creator A5028924440 @default.
• W3197206788 creator A5032719578 @default.
• W3197206788 creator A5083892118 @default.
• W3197206788 creator A5091101235 @default.
• W3197206788 date "2021-09-02" @default.
• W3197206788 modified "2023-10-17" @default.
• W3197206788 title "Geometry effects on dust attenuation curves with different grain sources at high redshift" @default.
• W3197206788 cites W1524555145 @default.
• W3197206788 cites W1569925696 @default.
• W3197206788 cites W1770723799 @default.
• W3197206788 cites W1848338669 @default.
• W3197206788 cites W1973808059 @default.
• W3197206788 cites W1974288578 @default.
• W3197206788 cites W1978009383 @default.
• W3197206788 cites W1980124829 @default.
• W3197206788 cites W1980842862 @default.
• W3197206788 cites W1986549462 @default.
• W3197206788 cites W1994671833 @default.
• W3197206788 cites W2000840256 @default.
• W3197206788 cites W2006869439 @default.
• W3197206788 cites W2007629416 @default.
• W3197206788 cites W2007993160 @default.
• W3197206788 cites W2008047915 @default.
• W3197206788 cites W2019103771 @default.
• W3197206788 cites W2029193721 @default.
• W3197206788 cites W2031826267 @default.
• W3197206788 cites W2037187722 @default.
• W3197206788 cites W2037732715 @default.
• W3197206788 cites W2045895958 @default.
• W3197206788 cites W2051661622 @default.
• W3197206788 cites W2053265856 @default.
• W3197206788 cites W2053781585 @default.
• W3197206788 cites W2055437312 @default.
• W3197206788 cites W2070696493 @default.
• W3197206788 cites W2072396470 @default.
• W3197206788 cites W2077678988 @default.
• W3197206788 cites W2077701059 @default.
• W3197206788 cites W2081521831 @default.
• W3197206788 cites W2085797005 @default.
• W3197206788 cites W2089167229 @default.
• W3197206788 cites W2090851853 @default.
• W3197206788 cites W2125956834 @default.
• W3197206788 cites W2126486572 @default.
• W3197206788 cites W2147181541 @default.
• W3197206788 cites W2151062050 @default.
• W3197206788 cites W2158567245 @default.
• W3197206788 cites W2169679801 @default.
• W3197206788 cites W2172214556 @default.
• W3197206788 cites W2409320150 @default.
• W3197206788 cites W2411031351 @default.
• W3197206788 cites W2425957420 @default.
• W3197206788 cites W2491291961 @default.
• W3197206788 cites W2501238181 @default.
• W3197206788 cites W2516068589 @default.
• W3197206788 cites W2555564993 @default.
• W3197206788 cites W2594398567 @default.
• W3197206788 cites W2612049161 @default.
• W3197206788 cites W2615876086 @default.
• W3197206788 cites W2661672368 @default.
• W3197206788 cites W2765132245 @default.
• W3197206788 cites W2765801315 @default.
• W3197206788 cites W2796170436 @default.
• W3197206788 cites W2806073152 @default.
• W3197206788 cites W2807643659 @default.
• W3197206788 cites W2897576229 @default.
• W3197206788 cites W2905489954 @default.
• W3197206788 cites W2917863768 @default.
• W3197206788 cites W2932280925 @default.
• W3197206788 cites W2937635485 @default.
• W3197206788 cites W2965883058 @default.
• W3197206788 cites W2974380898 @default.
• W3197206788 cites W2999332968 @default.
• W3197206788 cites W3004525215 @default.
• W3197206788 cites W3013188716 @default.
• W3197206788 cites W3016151600 @default.
• W3197206788 cites W3019338181 @default.
• W3197206788 cites W3019629504 @default.
• W3197206788 cites W3043687200 @default.
• W3197206788 cites W3090796811 @default.
• W3197206788 cites W3096872038 @default.
• W3197206788 cites W3097994407 @default.
• W3197206788 cites W3099524572 @default.
• W3197206788 cites W3099686071 @default.
• W3197206788 cites W3099742653 @default.
• W3197206788 cites W3099774793 @default.
• W3197206788 cites W3100024326 @default.
• W3197206788 cites W3100144206 @default.
• W3197206788 cites W3100345986 @default.
• W3197206788 cites W3101242588 @default.
• W3197206788 cites W3101256886 @default.
• W3197206788 cites W3101404470 @default.
• W3197206788 cites W3101498717 @default.
• W3197206788 cites W3101691828 @default.
• W3197206788 cites W3102033945 @default.
• W3197206788 cites W3102679327 @default.
• W3197206788 cites W3102956461 @default.

• next