Matches in SemOpenAlex for { <https://semopenalex.org/work/W4312037525> ?p ?o ?g. }
- W4312037525 endingPage "162" @default.
- W4312037525 startingPage "162" @default.
- W4312037525 abstract "We present a new derivation of the Milky Way's current star formation rate (SFR) based on the data of the Hi-GAL Galactic plane survey. We estimate the distribution of the SFR across the Galactic plane from the star-forming clumps identified in the Hi-GAL survey and calculate the total SFR from the sum of their contributions. The estimate of the global SFR amounts to $2.0 pm 0.7$~M$_{odot}$~yr$^{-1}$, of which $1.7 pm 0.6$~M$_{odot}$~yr$^{-1}$ coming from clumps with reliable heliocentric distance assignment. This value is in general agreement with estimates found in the literature of last decades. The profile of SFR density averaged in Galactocentric rings is found to be qualitatively similar to others previously computed, with a peak corresponding to the Central Molecular Zone and another one around Galactocentric radius $R_mathrm{gal} sim 5$~kpc, followed by an exponential decrease as $log(Sigma_mathrm{SFR}/[mathrm{M}_odot~mathrm{yr}^{-1}~mathrm{kpc}^{-2}])=a,R_mathrm{gal}/[mathrm{kpc}]+b $, with $a=-0.28 pm 0.01$. In this regard, the fraction of SFR produced within and outside the Solar circle is 84% and 16%, respectively; the fraction corresponding to the far outer Galaxy ($R_mathrm{gal} > 13.5$~kpc) is only 1%. We also find that, for $R_mathrm{gal}>3$~kpc, our data follow a power law as a function of density, similarly to the Kennicutt-Schmidt relation. Finally, we compare the distribution of the SFR density across the face-on Galactic plane and those of median parameters, such as temperature, luminosity/mass ratio and bolometric temperature, describing the evolutionary stage of Hi-GAL clumps. We found no clear correlation between the SFR and the clump evolutionary stage." @default.
- W4312037525 created "2023-01-04" @default.
- W4312037525 creator A5004073796 @default.
- W4312037525 creator A5008869887 @default.
- W4312037525 creator A5024095636 @default.
- W4312037525 creator A5027597083 @default.
- W4312037525 creator A5032225372 @default.
- W4312037525 creator A5036835022 @default.
- W4312037525 creator A5038039792 @default.
- W4312037525 creator A5038398980 @default.
- W4312037525 creator A5041690921 @default.
- W4312037525 creator A5042109641 @default.
- W4312037525 creator A5043821503 @default.
- W4312037525 creator A5046797058 @default.
- W4312037525 creator A5049559831 @default.
- W4312037525 creator A5057764147 @default.
- W4312037525 creator A5058607747 @default.
- W4312037525 creator A5060304964 @default.
- W4312037525 creator A5062809181 @default.
- W4312037525 creator A5064430529 @default.
- W4312037525 creator A5067983401 @default.
- W4312037525 creator A5070650240 @default.
- W4312037525 creator A5075623225 @default.
- W4312037525 creator A5078838333 @default.
- W4312037525 creator A5079635831 @default.
- W4312037525 creator A5085849603 @default.
- W4312037525 creator A5091564768 @default.
- W4312037525 creator A5091575644 @default.
- W4312037525 date "2022-12-01" @default.
- W4312037525 modified "2023-09-30" @default.
- W4312037525 title "The Star Formation Rate of the Milky Way as Seen by Herschel" @default.
- W4312037525 cites W1718032686 @default.
- W4312037525 cites W1796926725 @default.
- W4312037525 cites W1910578698 @default.
- W4312037525 cites W1934387688 @default.
- W4312037525 cites W1964344398 @default.
- W4312037525 cites W1964867136 @default.
- W4312037525 cites W1968137411 @default.
- W4312037525 cites W1998084400 @default.
- W4312037525 cites W2006878995 @default.
- W4312037525 cites W2007725308 @default.
- W4312037525 cites W2023409203 @default.
- W4312037525 cites W2032705382 @default.
- W4312037525 cites W2033223429 @default.
- W4312037525 cites W2034828518 @default.
- W4312037525 cites W2042523227 @default.
- W4312037525 cites W2047927543 @default.
- W4312037525 cites W2063882278 @default.
- W4312037525 cites W2063969444 @default.
- W4312037525 cites W2068967919 @default.
- W4312037525 cites W2075074183 @default.
- W4312037525 cites W2086284269 @default.
- W4312037525 cites W2090135680 @default.
- W4312037525 cites W2091990846 @default.
- W4312037525 cites W2096967293 @default.
- W4312037525 cites W2097928732 @default.
- W4312037525 cites W2099959892 @default.
- W4312037525 cites W2107052627 @default.
- W4312037525 cites W2108064551 @default.
- W4312037525 cites W2108220845 @default.
- W4312037525 cites W2116466430 @default.
- W4312037525 cites W2117237551 @default.
- W4312037525 cites W2121404382 @default.
- W4312037525 cites W2123267088 @default.
- W4312037525 cites W2135536375 @default.
- W4312037525 cites W2136310247 @default.
- W4312037525 cites W2140347367 @default.
- W4312037525 cites W2148681289 @default.
- W4312037525 cites W2151962171 @default.
- W4312037525 cites W2153312824 @default.
- W4312037525 cites W2155488926 @default.
- W4312037525 cites W2157128985 @default.
- W4312037525 cites W2162680201 @default.
- W4312037525 cites W2171508750 @default.
- W4312037525 cites W2216753448 @default.
- W4312037525 cites W2230493961 @default.
- W4312037525 cites W2331321138 @default.
- W4312037525 cites W2500628517 @default.
- W4312037525 cites W2513124424 @default.
- W4312037525 cites W2533579457 @default.
- W4312037525 cites W2556709513 @default.
- W4312037525 cites W2561153020 @default.
- W4312037525 cites W2575003957 @default.
- W4312037525 cites W2601507719 @default.
- W4312037525 cites W2606670595 @default.
- W4312037525 cites W2606765257 @default.
- W4312037525 cites W2620880236 @default.
- W4312037525 cites W2621520084 @default.
- W4312037525 cites W2755942060 @default.
- W4312037525 cites W2788110959 @default.
- W4312037525 cites W2798336535 @default.
- W4312037525 cites W2946130948 @default.
- W4312037525 cites W2949313893 @default.
- W4312037525 cites W2971471362 @default.
- W4312037525 cites W3083113835 @default.
- W4312037525 cites W3099723163 @default.
- W4312037525 cites W3099830973 @default.
- W4312037525 cites W3100106758 @default.