Matches in SemOpenAlex for { <https://semopenalex.org/work/W2080481182> ?p ?o ?g. }
- W2080481182 endingPage "A8" @default.
- W2080481182 startingPage "A8" @default.
- W2080481182 abstract "Context. Measuring star formation at a local scale is important to constrain star formation laws. Yet, it is not clear whether and how the measure of star formation is affected by the spatial scale at which a galaxy is observed. Aims. We want to understand the impact of the resolution on the determination of the spatially resolved star formation rate (SFR) and other directly associated physical parameters such as the attenuation. Methods. We have carried out a multi-scale, pixel-by-pixel study of the nearby galaxy M33. Assembling FUV, Halpha, 8, 24, 70, and 100 micron maps, we have systematically compared the emission in individual bands with various SFR estimators from a resolution of 33 pc to 2084 pc. Results. We have found that there are strong, scale-dependent, discrepancies up to a factor 3 between monochromatic SFR estimators and Halpha+24 micron. The scaling factors between individual IR bands and the SFR show a strong dependence on the spatial scale and on the intensity of star formation. Finally, strong variations of the differential reddening between the nebular emission and the stellar continuum are seen, depending on the specific SFR (sSFR) and on the resolution. At the finest spatial scales, there is little differential reddening at high sSFR. The differential reddening increases with decreasing sSFR. At the coarsest spatial scales the differential reddening is compatible with the canonical value found for starburst galaxies. Conclusions. Our results confirm that monochromatic estimators of the SFR are unreliable at scales smaller than 1 kpc. Furthermore, the extension of local calibrations to high redshift galaxies presents non-trivial challenges as the properties of these systems may be poorly known." @default.
- W2080481182 created "2016-06-24" @default.
- W2080481182 creator A5000008228 @default.
- W2080481182 creator A5003825811 @default.
- W2080481182 creator A5004342345 @default.
- W2080481182 creator A5010717725 @default.
- W2080481182 creator A5011914272 @default.
- W2080481182 creator A5013399155 @default.
- W2080481182 creator A5021911720 @default.
- W2080481182 creator A5031303202 @default.
- W2080481182 creator A5035243411 @default.
- W2080481182 creator A5038687208 @default.
- W2080481182 creator A5043892757 @default.
- W2080481182 creator A5053724573 @default.
- W2080481182 creator A5061165927 @default.
- W2080481182 creator A5064812526 @default.
- W2080481182 creator A5067736707 @default.
- W2080481182 creator A5080091223 @default.
- W2080481182 creator A5082826821 @default.
- W2080481182 creator A5084364688 @default.
- W2080481182 date "2015-05-22" @default.
- W2080481182 modified "2023-10-18" @default.
- W2080481182 title "Measuring star formation with resolved observations: the test case of M 33" @default.
- W2080481182 cites W1507716615 @default.
- W2080481182 cites W1592218820 @default.
- W2080481182 cites W1684711259 @default.
- W2080481182 cites W1771831270 @default.
- W2080481182 cites W1833860403 @default.
- W2080481182 cites W1970279044 @default.
- W2080481182 cites W1971512060 @default.
- W2080481182 cites W1972562723 @default.
- W2080481182 cites W1974174849 @default.
- W2080481182 cites W1976879631 @default.
- W2080481182 cites W1982507072 @default.
- W2080481182 cites W1985386646 @default.
- W2080481182 cites W1991559510 @default.
- W2080481182 cites W1996537612 @default.
- W2080481182 cites W2000933741 @default.
- W2080481182 cites W2002038882 @default.
- W2080481182 cites W2005276762 @default.
- W2080481182 cites W2006878995 @default.
- W2080481182 cites W2012919097 @default.
- W2080481182 cites W2015733060 @default.
- W2080481182 cites W2016201661 @default.
- W2080481182 cites W2016847354 @default.
- W2080481182 cites W2017364885 @default.
- W2080481182 cites W2018657673 @default.
- W2080481182 cites W2019611731 @default.
- W2080481182 cites W2029842890 @default.
- W2080481182 cites W2044669640 @default.
- W2080481182 cites W2045895958 @default.
- W2080481182 cites W2048274049 @default.
- W2080481182 cites W2048340294 @default.
- W2080481182 cites W2050324272 @default.
- W2080481182 cites W2052923345 @default.
- W2080481182 cites W2055518619 @default.
- W2080481182 cites W2058387099 @default.
- W2080481182 cites W2063969444 @default.
- W2080481182 cites W2068234997 @default.
- W2080481182 cites W2068950512 @default.
- W2080481182 cites W2073949454 @default.
- W2080481182 cites W2082043166 @default.
- W2080481182 cites W2083821946 @default.
- W2080481182 cites W2084981136 @default.
- W2080481182 cites W2086201611 @default.
- W2080481182 cites W2088536005 @default.
- W2080481182 cites W2090135680 @default.
- W2080481182 cites W2090482424 @default.
- W2080481182 cites W2102351316 @default.
- W2080481182 cites W2104696574 @default.
- W2080481182 cites W2108240489 @default.
- W2080481182 cites W2111817932 @default.
- W2080481182 cites W2120031672 @default.
- W2080481182 cites W2121359722 @default.
- W2080481182 cites W2123267088 @default.
- W2080481182 cites W2133735951 @default.
- W2080481182 cites W2135625048 @default.
- W2080481182 cites W2138302982 @default.
- W2080481182 cites W2143213816 @default.
- W2080481182 cites W2146026248 @default.
- W2080481182 cites W2148804397 @default.
- W2080481182 cites W2151062050 @default.
- W2080481182 cites W2155593555 @default.
- W2080481182 cites W2167635287 @default.
- W2080481182 cites W2167774867 @default.
- W2080481182 cites W3098197335 @default.
- W2080481182 cites W3099103481 @default.
- W2080481182 cites W3099752361 @default.
- W2080481182 cites W3099992046 @default.
- W2080481182 cites W3100253958 @default.
- W2080481182 cites W3100908599 @default.
- W2080481182 cites W3101235820 @default.
- W2080481182 cites W3101256886 @default.
- W2080481182 cites W3101554889 @default.
- W2080481182 cites W3101582467 @default.
- W2080481182 cites W3102623908 @default.
- W2080481182 cites W3103325292 @default.
- W2080481182 cites W3104416848 @default.