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dc.contributorINAF-Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, I-00133 Roma, Italy
dc.contributorDepartamento de Astronomía, Universidad de Chile, Casilla 36-D, Correo Central, Santiago, Chile
dc.contributorAix Marseille Univ., CNRS, CNES, LAM, Marseille, France
dc.contributorScience & Technology Corporation, Olof Palmestraat 14, 2616 LR Delft, The Netherlands
dc.contributorAix Marseille Univ., CNRS, CNES, LAM, Marseille, France; Institut Universitaire de France, Paris, France
dc.contributorSpace Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA
dc.contributorINAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125, Firenze, Italy
dc.contributorUniversité Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, F-91191, Gif-sur-Yvette, France
dc.contributorUniversität Heidelberg, Zentrum für Astronomie, Institut für theoretische Astrophysik, Albert-Ueberle-Str. 2, D-69120 Heidelberg, Germany; Universität Heidelberg, Interdiszipliäres Zentrum für Wissenschaftliches Rechnen, Im Neuenheimer Feld 205, D-69120 Heidelberg, Germany
dc.contributorINAF-Osservatorio Astronomico di Cagliari, Via della Scienza 5, I-09047 Selargius (CA), Italy
dc.contributorInfrared Processing Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA
dc.contributorAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool, L3 5RF, UK; Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DB, UK
dc.contributorCanadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON, M5S 3H8, Canada
dc.contributorUniversität Heidelberg, Zentrum für Astronomie, Institut für theoretische Astrophysik, Albert-Ueberle-Str. 2, D-69120 Heidelberg, Germany
dc.contributorINAF-Istituto di Astrofisica e Planetologia Spaziali, Via Fosso del Cavaliere 100, I-00133 Roma, Italy; Dipartimento di Fisica, Sapienza Università di Roma, Piazzale Aldo Moro 2, I-00185, Rome, Italy
dc.contributorDepartment of Physics & Astronomy, University of Calgary, 2500 University Dr. NW, Calgary, AB, T2N 1N4, Canada
dc.contributor.authorElia, D.
dc.contributor.authorMolinari, S.
dc.contributor.authorSchisano, E.
dc.contributor.authorSoler, J. D.
dc.contributor.authorMerello, M.
dc.contributor.authorRusseil, D.
dc.contributor.authorVeneziani, M.
dc.contributor.authorZavagno, A.
dc.contributor.authorNoriega-Crespo, A.
dc.contributor.authorOlmi, L.
dc.contributor.authorBenedettini, M.
dc.contributor.authorHennebelle, P.
dc.contributor.authorKlessen, R. S.
dc.contributor.authorLeurini, S.
dc.contributor.authorPaladini, R.
dc.contributor.authorPezzuto, S.
dc.contributor.authorTraficante, A.
dc.contributor.authorEden, D. J.
dc.contributor.authorMartin, P. G.
dc.contributor.authorSormani, M.
dc.contributor.authorColetta, A.
dc.contributor.authorColman, T.
dc.contributor.authorPlume, R.
dc.contributor.authorMaruccia, Y.
dc.contributor.authorMininni, C.
dc.contributor.authorLiu, S. J.
dc.date.accessioned2024-02-02T13:30:41Z
dc.date.available2024-02-02T13:30:41Z
dc.date.issued2022-12-01T00:00:00Z
dc.identifier.doi10.3847/1538-4357/aca27d
dc.identifier.doi10.48550/arXiv.2211.05573
dc.identifier.other2022arXiv221105573E
dc.identifier.otherastro-ph.GA
dc.identifier.other2022arXiv221105573E
dc.identifier.other2022ApJ...941..162E
dc.identifier.otherarXiv:2211.05573
dc.identifier.other10.3847/1538-4357/aca27d
dc.identifier.other10.48550/arXiv.2211.05573
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dc.identifier.urihttp://hdl.handle.net/20.500.14302/1538
dc.description.abstractWe present a new derivation of the Milky Way's current star formation rate (SFR) based on the data of the Herschel InfraRed Galactic Plane Survey (Hi-GAL). 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 ± 0.7 M <SUB>⊙</SUB> yr<SUP>-1</SUP>, of which 1.7 ± 0.6 M <SUB>⊙</SUB> yr<SUP>-1</SUP> 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 <SUB>gal</SUB> ~ 5 kpc, followed by an exponential decrease as $\mathrm{log}({{\rm{\Sigma }}}_{\mathrm{SFR}}/[{M}_{\odot }\,{\mathrm{yr}}^{-1}\,{\mathrm{kpc}}^{-2}])=a\,{R}_{\mathrm{gal}}/[\mathrm{kpc}]+b$ , with a = -0.28 ± 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 <SUB>gal</SUB> &gt; 13.5 kpc) is only 1%. We also find that, for R <SUB>gal</SUB> &gt; 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.
dc.publisherThe Astrophysical Journal
dc.titleThe Star Formation Rate of the Milky Way as Seen by Herschel
dc.typearticle
dc.source.journalApJ
dc.source.journalApJ...941
dc.source.volume941
refterms.dateFOA2024-02-02T13:30:41Z
dc.identifier.bibcode2022ApJ...941..162E


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