The Star Formation Rate of the Milky Way as Seen by Herschel
Creators
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Elia, D.1
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Molinari, S.1
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Schisano, E.1
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Soler, J. D.1
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Merello, M.2
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Russeil, D.3
- Veneziani, M.4
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Zavagno, A.3, 5
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Noriega-Crespo, A.6
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Olmi, L.7
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Benedettini, M.1
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Hennebelle, P.8
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Klessen, R. S.9
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Leurini, S.
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Paladini, R.10
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Pezzuto, S.1
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Traficante, A.1
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Eden, D. J.11, 12
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Martin, P. G.13
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Sormani, M.9
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Coletta, A.1, 14
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Colman, T.8
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Plume, R.15
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Maruccia, Y.1
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Mininni, C.1
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Liu, S. J.1
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1.
National Institute for Astrophysics
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University of Chile
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3.
French National Centre for Scientific Research
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4.
Science and Technology Corporation (Netherlands)
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5.
Institut Universitaire de France
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Space Telescope Science Institute
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Arcetri Astrophysical Observatory
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University of Paris
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Heidelberg University
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Infrared Processing and Analysis Center
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11.
Liverpool John Moores University
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12.
Armagh Observatory
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13.
Canadian Institute for Theoretical Astrophysics
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14.
Sapienza University of Rome
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15.
University of Calgary
Abstract
We 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_⊙ yr⁻¹, of which 1.7 ± 0.6 M_⊙ 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_gal ∼ 5 kpc, followed by an exponential decrease as log(Σ_(SFR)/[M_⊙ yr⁻¹ kpc⁻²]) = a R_gal/[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_gal > 13.5 kpc) is only 1%. We also find that, for R_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.
Additional Information
This research has received funding from the INAF Mainstream Grant "The ultimate exploitation of the Hi-GAL archive and ancillary infrared/mm data" (1.05.01.86.09), and from the European Research Council synergy grant ECOGAL (grant No. 855130). S.L. acknowledges support by the INAF PRIN 2019 grant ONSET. A.Z. thanks the support of the Institut Universitaire de France.Additional details
Identifiers
- Eprint ID
- 118745
- Resolver ID
- CaltechAUTHORS:20230105-911538600.8
Funding
- Istituto Nazionale di Astrofisica (INAF)
- 1.05.01.86.09
- European Research Council (ERC)
- 855130
- Institut Universitaire de France (IUF)
Dates
- Created
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2023-02-08Created from EPrint's datestamp field
- Updated
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2023-02-08Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)