Response to Sierra-Delgado et al.

Geyter, Christian De; M’Rabet, Nadira; Geyter, Julie De; Hong, Zhang; Heinimann, Karl

doi:10.1038/gim.2016.79

Cited by 7 publications

(8 citation statements)

References 4 publications

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“…These characteristics have been first derived from modelling edgeon galaxies by Xilouris et al (1997Xilouris et al ( , 1998Xilouris et al ( , 1999, and have been used and shown to account for the panchromatic modelling of edgeon galaxies in Popescu et al (2000a), Misiriotis et al (2001) and Popescu et al (2004), and adopted in our generic model of PT11. Further studies made by other groups have also confirmed these characteristics (Bianchi & Xilouris 2011, Schechtman-Rook et al 2012, De Geyter et al 2013. As we will show in this paper, these characteristics are found to be exhibited by the dust disk of the Milky Way as well.…”

supporting

confidence: 77%

A radiation transfer model for the Milky Way. II The global properties and large scale structure

Natale,

Popescu,

Rushton

et al. 2021

Preprint

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We obtained an axi-symmetric model for the large-scale distribution of stars and dust in the Milky Way (MW) using a radiative transfer code that can account for the existing near-infrared (NIR)/mid-infrared/submm all-sky emission maps of our Galaxy. We find that the MW has a star-formation rate of SFR = 1.25 ± 0.2 M /yr, a stellar mass 𝑀 * = (4.9 ± 0.3) × 10 10 M , and a specific SFR that is relatively constant with radius (except for the inner 1 kpc). We identified an inner radius 𝑅 in = 4.5 kpc beyond which the stellar emissivity and dust distribution fall exponentially. For 𝑅 < 𝑅 in the emissivities fall linearly towards the centre. The old stellar populations in the disk have an exponential scalelength that increases monotonically from ℎ disk s (𝐾) = 2.2 ± 0.6 kpc in the NIR, to ℎ disk s (𝐵) = 3.2 ± 0.9 kpc at the shorter optical bands, and a scaleheight that varies with radial distance, from 𝑧 disk s (0) = 140 ± 20 pc in the centre to 𝑧 disk s (𝑅 ) = 300 ± 20 pc at the solar radius. The young stellar populations have a scalelength of ℎ tdisk s = 3.2 ± 0.9 kpc and a scaleheight that varies from 𝑧 tdisk s (0) = 50 ± 10 pc in the centre to 𝑧 tdisk s (𝑅 ) = 90±10 pc at the solar radius. We discovered an inner stellar disk within the central 4.5 kpc, which we associate with the extended long bar of the MW. Most of the obscured star formation happens within this inner thin disk. The diffuse dust is mainly distributed in a disk with scalelength ℎ disk d = 5.2 ± 0.8 kpc and scaleheight 𝑧 disk d = 0.14 ± 0.02 kpc. We give the first derivation of the MW attenuation curve and present it as a functional fit to the model data. We find the MW to lie in the Green Valley of the main sequence relation for spiral galaxies.

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supporting

confidence: 77%

A radiation transfer model for the Milky Way. II The global properties and large scale structure

Natale,

Popescu,

Rushton

et al. 2021

Preprint

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“…De Geyter et al 2013. As we will show in this paper, these characteristics are found to be exhibited by the dust disk of the Milky Way as well.…”

supporting

confidence: 58%

A radiation transfer model for the Milky Way. II The global properties and large scale structure

Natale

Popescu

Rushton

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We obtained an axi-symmetric model for the large-scale distribution of stars and dust in the Milky Way (MW) using a radiative transfer code that can account for the existing near-infrared (NIR)/mid-infrared/submm all-sky emission maps of our Galaxy. We find that the MW has a star-formation rate of SFR = 1.25 ± 0.2 M⊙/yr, a stellar mass M* = (4.9 ± 0.3) × 1010 M⊙, and a specific SFR that is relatively constant with radius (except for the inner 1 kpc). We identified an inner radius Rin = 4.5 kpc beyond which the stellar emissivity and dust distribution fall exponentially. For R < Rin the emissivities fall linearly towards the centre. The old stellar populations in the disk have an exponential scalelength that increases monotonically from $h_{\rm s}^{\rm disk}(K)=2.2\pm 0.6$ kpc in the NIR, to $h_{\rm s}^{\rm disk}(B)=3.2\pm 0.9$ kpc at the shorter optical bands, and a scaleheight that varies with radial distance, from $z_{\rm s}^{\rm disk}(0) =140\pm 20$ pc in the centre to $z_{\rm s}^{\rm disk}(R_{\odot }) =300\pm 20$ pc at the solar radius. The young stellar populations have a scalelength of $h_{\rm s}^{\rm tdisk}=3.2\pm 0.9$ kpc and a scaleheight that varies from $z_{\rm s}^{\rm tdisk}(0)=50\pm 10$ pc in the centre to $z_{\rm s}^{\rm tdisk}(R_{\odot })=90\pm 10$ pc at the solar radius. We discovered an inner stellar disk within the central 4.5 kpc, which we associate with the extended long bar of the MW. Most of the obscured star formation happens within this inner thin disk. The diffuse dust is mainly distributed in a disk with scalelength $h_{\rm d}^{\rm disk}=5.2\pm 0.8$ kpc and scaleheight $z_{\rm d}^{\rm disk}=0.14\pm 0.02$ kpc. We give the first derivation of the MW attenuation curve and present it as a functional fit to the model data. We find the MW to lie in the Green Valley of the main sequence relation for spiral galaxies.

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“…In the LMC (Galliano et al 2011), the far-IR grain emissivity is found to be 2-3 times higher than in the widely used prescription of Draine & Li (2007) which fits data for the Milky Way (Planck Collaboration 2014). Detailed panchromatic radiative transfer studies of edge-on spiral galaxies point in a similar direction (Baes et al 2011;De Geyter et al 2015;Mosenkov et al 2016). Getting the dust emissivity correct throughout the mid-to far-IR is essential to estimate extinctions at optical/UV wave-lengths, which are key to derive stellar masses and SFRs.…”

Section: Dust Content Of Nearby Galaxiesmentioning

confidence: 96%

Probing the Baryon Cycle of Galaxies with SPICA Mid- and Far-Infrared Observations

Tak

Madden

Roelfsema

et al. 2018

Publ. Astron. Soc. Aust.

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The SPICA mid and far-infrared telescope will address fundamental issues in our understanding of star formation and ISM physics in galaxies. A particular hallmark of SPICA is the outstanding sensitivity enabled by the cold telescope, optimized detectors, and wide instantaneous bandwidth throughout the midand far-infrared. The spectroscopic, imaging and polarimetric observations that SPICA will be able to collect will help in clarifying the complex physical mechanisms which underlie the baryon cycle of galaxies. In particular: (i) The access to a large suite of atomic and ionic fine-structure lines for large samples of galaxies will shed light on the origin of the observed spread in star formation rates within and between galaxies. (ii) Observations of HD rotational lines (out to ∼10 Mpc) and fine structure lines such as [C ii] 158 µm (out to ∼100 Mpc) will clarify the main reservoirs of interstellar matter in galaxies, including phases where CO does not emit. (iii) Far-infrared spectroscopy of dust and ice features will address uncertainties in the mass and composition of dust in galaxies, and the contributions of supernovae to the interstellar dust budget will be quantified by photometry and monitoring of supernova remnants in nearby galaxies. (iv) Observations of far-infrared cooling lines such as [O i] 63 µm from star-forming molecular clouds in our Galaxy will evaluate the importance of shocks to dissipate turbulent energy. The paper concludes with requirements for the telescope and instruments, and recommendations for the observing strategy.

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Response to Sierra-Delgado et al.

Cited by 7 publications

References 4 publications

A radiation transfer model for the Milky Way. II The global properties and large scale structure

A radiation transfer model for the Milky Way. II The global properties and large scale structure

A radiation transfer model for the Milky Way. II The global properties and large scale structure

Probing the Baryon Cycle of Galaxies with SPICA Mid- and Far-Infrared Observations

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