FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W3100743064> ?p ?o ?g. }

• W3100743064 endingPage "A4" @default.
• W3100743064 startingPage "A4" @default.
• W3100743064 abstract "The spectral energy distributions (SEDs) of low-mass low-metallicity (dwarf) galaxies are a challenging piece of the puzzle of galaxy formation in the near Universe. These SEDs show some particular features in the submillimeter to far-infrared wavelength range compared to normal, larger, and metal-richer galaxies that cannot be explained by the current models. These can be summarized as: a broadening of the IR peak, which implies a warmer dust component; an excess of emission in the submm ($sim$500 $mu$m), that causes a flattening of the submm/FIR slope; and a very low intensity of PAH emission features. With the aim of explaining these emission patterns, the SEDs of a sample of 27 simulated dwarf galaxies were calculated using the GRASIL-3D radiation transfer code. This code has the particularity that it separately treats the radiative transfer through dust grains within molecular clouds and within the cirrus, the dense and diffuse components of the gas phase, respectively. The simulated galaxies have stellar masses ranging from 10$^6$-10$^9$ M$_odot$, and were obtained from a single simulation run within a Local Group environment with initial conditions from the CLUES project. We report a study of the IRAS, Spitzer and Herschel bands luminosities, and of the SFRs, dust, and gas (HI and H$_2$) mass contents. We find a satisfactory agreement with observational data, with GRASIL-3D naturally reproducing the specific spectral features mentioned above. We conclude that the GRASIL-3D two-component dust model gives a physical interpretation of the emission of dwarf galaxies: molecular clouds and cirrus represent the warm and cold dust components, respectively, needed to reproduce observational data." @default.
• W3100743064 created "2020-11-23" @default.
• W3100743064 creator A5003126790 @default.
• W3100743064 creator A5031672588 @default.
• W3100743064 creator A5046985258 @default.
• W3100743064 creator A5059730518 @default.
• W3100743064 creator A5062813609 @default.
• W3100743064 date "2017-06-30" @default.
• W3100743064 modified "2023-10-17" @default.
• W3100743064 title "Diversity of dwarf galaxy IR-submm emission patterns: CLUES from hydrodynamical simulations" @default.
• W3100743064 cites W1498399178 @default.
• W3100743064 cites W1545762935 @default.
• W3100743064 cites W1912314976 @default.
• W3100743064 cites W1929623410 @default.
• W3100743064 cites W1943043803 @default.
• W3100743064 cites W1952356865 @default.
• W3100743064 cites W1964844412 @default.
• W3100743064 cites W1964925572 @default.
• W3100743064 cites W1967037459 @default.
• W3100743064 cites W1971512060 @default.
• W3100743064 cites W1973808059 @default.
• W3100743064 cites W1973833544 @default.
• W3100743064 cites W1975524662 @default.
• W3100743064 cites W1977843574 @default.
• W3100743064 cites W1980924370 @default.
• W3100743064 cites W1986163712 @default.
• W3100743064 cites W1986959020 @default.
• W3100743064 cites W1987522415 @default.
• W3100743064 cites W1989498292 @default.
• W3100743064 cites W1991391334 @default.
• W3100743064 cites W1993867049 @default.
• W3100743064 cites W1994174531 @default.
• W3100743064 cites W1994730148 @default.
• W3100743064 cites W2002038882 @default.
• W3100743064 cites W2002726510 @default.
• W3100743064 cites W2003637061 @default.
• W3100743064 cites W2004311301 @default.
• W3100743064 cites W2005582416 @default.
• W3100743064 cites W2007442140 @default.
• W3100743064 cites W2007993160 @default.
• W3100743064 cites W2013921589 @default.
• W3100743064 cites W2013965924 @default.
• W3100743064 cites W2014678453 @default.
• W3100743064 cites W2015267403 @default.
• W3100743064 cites W2018396757 @default.
• W3100743064 cites W2018657673 @default.
• W3100743064 cites W2021195299 @default.
• W3100743064 cites W2029193721 @default.
• W3100743064 cites W2032072360 @default.
• W3100743064 cites W2032921984 @default.
• W3100743064 cites W2034535798 @default.
• W3100743064 cites W2034608771 @default.
• W3100743064 cites W2035198704 @default.
• W3100743064 cites W2038517717 @default.
• W3100743064 cites W2040993126 @default.
• W3100743064 cites W2041561966 @default.
• W3100743064 cites W2042956136 @default.
• W3100743064 cites W2043452159 @default.
• W3100743064 cites W2044561508 @default.
• W3100743064 cites W2045491779 @default.
• W3100743064 cites W2046061553 @default.
• W3100743064 cites W2047798125 @default.
• W3100743064 cites W2047894542 @default.
• W3100743064 cites W2048274049 @default.
• W3100743064 cites W2049062775 @default.
• W3100743064 cites W2051661622 @default.
• W3100743064 cites W2052923345 @default.
• W3100743064 cites W2056076677 @default.
• W3100743064 cites W2067813516 @default.
• W3100743064 cites W2069524830 @default.
• W3100743064 cites W2070040541 @default.
• W3100743064 cites W2072088379 @default.
• W3100743064 cites W2073147034 @default.
• W3100743064 cites W2075292617 @default.
• W3100743064 cites W2077017611 @default.
• W3100743064 cites W2078858012 @default.
• W3100743064 cites W2080224591 @default.
• W3100743064 cites W2083576610 @default.
• W3100743064 cites W2090135680 @default.
• W3100743064 cites W2098000362 @default.
• W3100743064 cites W2098620773 @default.
• W3100743064 cites W2100452140 @default.
• W3100743064 cites W2104696574 @default.
• W3100743064 cites W2107833181 @default.
• W3100743064 cites W2116466430 @default.
• W3100743064 cites W2123267088 @default.
• W3100743064 cites W2123480589 @default.
• W3100743064 cites W2127979873 @default.
• W3100743064 cites W2129153205 @default.
• W3100743064 cites W2131462302 @default.
• W3100743064 cites W2133308199 @default.
• W3100743064 cites W2136336431 @default.
• W3100743064 cites W2138282692 @default.
• W3100743064 cites W2141530767 @default.
• W3100743064 cites W2142471547 @default.
• W3100743064 cites W2143988162 @default.
• W3100743064 cites W2153107905 @default.
• W3100743064 cites W2155421027 @default.

• next