The<i>Herschel</i>Exploitation of Local Galaxy Andromeda (HELGA)

Viaene, S.; Baes, M.; Tamm, A.; Tempel, Elmo; Bendo, G. J.; Blommaert, J. A. D. L.; Boquien, M.; Boselli, A.; Camps, Peter; Cooray, Asantha; Looze, I. De; Vis, P. De; Fernández-Ontiveros, J. A.; Fritz, J.; Galametz, M.; Gentile, Gianfranco; Madden, S.; Smith, M.; Spinoglio, L.; Verstocken, Sam

doi:10.1051/0004-6361/201629251

Cited by 73 publications

(127 citation statements)

References 140 publications

(162 reference statements)

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“…It is immediately apparent that M33's attenuation curve is much steeper in the UV than the Milky Way extinction curve (if both curves are normalised in the B-band). Similar results have been obtained in the RT modelling of M51 (De Looze et al 2014) and of M31 (Viaene et al 2017). Another interesting feature of the attenuation curve is the 2200Å bump, which for M33 is deeper than in the MW extinction curve.…”

Section: The Attenuation Curve Of M33supporting

confidence: 85%

“…More recently efforts started to be devoted to modelling face-on galaxies, in particular driven by the recent availability of high resolution panchromatic images, including those in the important FIR/submm regime. First attempts have been done in De Looze et al (2014), Viaene et al (2017), and Williams et al (2019) using non-axi-symmetric RT models. However, because of their non-axi-symmetric nature and the way they are implemented, they were not used to fit the geometry of the system, due to the prohibited computational time, but only used to fit the spatially integrated SEDs.…”

Section: ;mentioning

confidence: 99%

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A radiative transfer model for the spiral galaxy M33★

Thirlwall

Popescu

Tuffs

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the first radiative transfer (RT) model of a non-edge-on disk galaxy in which the large-scale geometry of stars and dust is self-consistently derived through fitting of multiwavelength imaging observations from the UV to the submm. To this end we used the axi-symmetric RT model of Popescu et al. and a new methodology for deriving geometrical parameters, and applied this to decode the spectral energy distribution (SED) of M33. We successfully account for both the spatial and spectral energy distribution, with residuals typically within 7% in the profiles of surface brightness and within 8% in the spatially-integrated SED. We predict well the energy balance between absorption and re-emission by dust, with no need to invoke modified grain properties, and we find no submm emission that is in excess of our model predictions. We calculate that 80 ± 8% of the dust heating is powered by the young stellar populations. We identify several morphological components in M33, a nuclear, an inner, a main and an outer disc, showing a monotonic trend in decreasing star-formation surface-density (Σ SFR ) from the nuclear to the outer disc. In relation to surface density of stellar mass, the Σ SFR of these components define a steeper relation than the "main sequence" of star-forming galaxies, which we call a "structurally resolved main sequence". Either environmental or stellar feedback mechanisms could explain the slope of the newly defined sequence. We find the star-formation rate to be SFR = 0.28 +0.02 −0.01 M yr −1 .

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Section: The Attenuation Curve Of M33supporting

confidence: 85%

Section: ;mentioning

confidence: 99%

A radiative transfer model for the spiral galaxy M33★

Thirlwall

Popescu

Tuffs

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Multiple results indicate the need for more complex dust distribution models within galaxies in order to match simulations and observations (Wong & Blitz 2002, Popescu et al 2011, Viaene et al 2017. Wong & Blitz (2002) proposed a "hybrid" model where dust behaves differently in region located in the center/inner and outer disk of galaxies.…”

Section: 21)mentioning

confidence: 99%

Attenuation Modified by DIG and Dust as Seen in M31

Tomičić

Kreckel

Groves

et al. 2017

ApJ

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The spatial distribution of dust in galaxies affects the global attenuation, and hence inferred properties, of galaxies. We trace the spatial distribution of dust in five fields (at 0.6-0.9 kpc scale) of M31 by comparing optical attenuation with the total dust mass distribution. We measure the attenuation from the Balmer decrement using Integral Field Spectroscopy and the dust mass from Herschel far-IR observations. Our results show that M31's dust attenuation closely follows a foreground screen model, contrary to what was previously found in other nearby galaxies. By smoothing the M31 data we find that spatial resolution is not the cause for this difference. Based on the emission line ratios and two simple models, we conclude that previous models of dust/gas geometry need to include a weakly or non-attenuated diffuse ionized gas (DIG) component. Due to the variation of dust and DIG scale heights with galactic radius, we conclude that different locations in galaxies will have different vertical distributions of gas and dust and therefore different measured attenuation. The difference between our result in M31 with that found in other nearby galaxies can be explained by our fields in M31 lying at larger galactic radii than the previous studies that focused on the centers of galaxies.

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“…The direct mapping from plane of the sky to plane of the galaxy makes the implicit assumption of an infinitely thin disc, but is also a reasonable approximation for low inclination angles. Viaene et al (2017) have even achieved realistic de-projection results for M 31 with an inclination angle of 77.5 • . We base our estimated inclination angle for M 81 on the apparent flattening of the disc found by the S 4 G decomposition, using the Hubble formula (Hubble 1926):…”

Section: The Stellar Bulgementioning

confidence: 89%

“…This non-local character of dust heating might be important (Smith & Hayward 2015;Boquien et al 2015). 3D radiative transfer analyses have demonstrated the non-locality of dust heating in the Sombrero galaxy De Looze et al (2012b) and the Andromeda galaxy (Viaene et al 2017). In both galaxies, the radiation from the old stellar populations in the bulge has proven to propagate far outwards and contribute to the heating out to large distances.…”

Section: Introductionmentioning

confidence: 99%

High-resolution, 3D radiative transfer modelling

Verstocken

Nersesian

Baes

et al. 2020

A&A

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Context. Interstellar dust absorbs stellar light very efficiently and thus shapes the energetic output of galaxies. Studying the impact of different stellar populations on the dust heating remains hard because it requires decoupling the relative geometry of stars and dust, and involves complex processes as scattering and non-local dust heating. Aims. We aim to constrain the relative distribution of dust and stellar populations in the spiral galaxy M 81 and create a realistic model of the radiation field that describes the observations. Investigating the dust-starlight interaction on local scales, we want to quantify the contribution of young and old stellar populations to the dust heating. We aim to standardise the setup and model selection of such inverse radiative transfer simulations so this can be used for comparable modelling of other nearby galaxies. Methods. We present a semi-automated radiative transfer modelling pipeline that implements the necessary steps such as the geometric model construction and the normalisation of the components through an optimisation routine. We use the Monte Carlo radiative transfer code SKIRT to calculate a self-consistent, panchromatic model of the interstellar radiation field. By looking at different stellar populations independently, we can quantify to what extent different stellar age populations contribute to the dust heating. Our method takes into account the effects of non-local heating. Results. We obtain a realistic 3D radiative transfer model of the face-on galaxy M 81. We find that only 50.2% of the dust heating can be attributed to young stellar populations ( 100 Myr). We confirm a tight correlation between the specific star formation rate and the heating fraction by young stellar populations, both in sky projection and in 3D, also found for radiative transfer models of M 31 and M 51. Conclusions. We conclude that the old stellar populations can be a major contributor to the heating of dust. In M 81, old stellar populations are the dominant heating agent in the central regions and they contribute to half of the absorbed radiation. Regions of higher star formation do not correspond to the highest dust temperatures. On the contrary, it is the dominant bulge which is most efficient in heating the dust. The approach we present here can immediately be applied to other galaxies. It does contain a number of caveats which are discussed in detail.

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TheHerschelExploitation of Local Galaxy Andromeda (HELGA)

Cited by 73 publications

References 140 publications

A radiative transfer model for the spiral galaxy M33★

A radiative transfer model for the spiral galaxy M33★

Attenuation Modified by DIG and Dust as Seen in M31

High-resolution, 3D radiative transfer modelling

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