Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Casasola, V.; Cassarà, L. P.; Bianchi, S.; Verstocken, Sam; Xilouris, E. M.; Magrini, L.; Smith, M.; Looze, I. De; Galametz, M.; Madden, S.; Baes, M.; Clark, Christopher; Davies, J.; Vis, P. De; Evans, R.; Fritz, J.; Galliano, F.; Jones, A. P.; Mosenkov, Aleksandr V.; Viaene, S.; Ysard, N.

doi:10.1051/0004-6361/201731020

Cited by 131 publications

(163 citation statements)

References 189 publications

Supporting

Mentioning

145

Contrasting

Order By: Relevance

“…Calistro Rivera et al (2018) showed how the (apparent) compactness of the dust can be explained by a radial decrease of the gas column density and dust temperature toward the outskirts of the sources, on the basis of a radiative transfer model presented by Weiß et al (2007). It is interesting to note that Casasola et al (2017), analysing the gas and dust distribution of a sample of 18 nearby face-on galaxies, found that -on average-the exponential scale-length of the dust-mass surfacedensity is ∼2.3 times higher than that of the molecular gas, that is the dust is distributed at larger radii than the molecular gas, contrary to what we found at high-z. However, we point out that given the sensitivity limit of our observation it is possible that we are tracing only the innermost, warmer phase of dust, whose emission flux increases linearly with the density and temperature (in the Rayleigh-Jeans regime, assuming a constant dust mass).…”

Section: Source Sizecontrasting

confidence: 98%

Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

D’Amato

Gilli²,

Vignali³

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

Context. Obscured active galactic nuclei (AGN) represent a significant fraction of the entire AGN population, especially at high redshift (∼70% at z=3-5). They are often characterized by the presence of large gas and dust reservoirs that are thought to sustain and possibly obscure vigorous star formation processes that make these objects shine at far-IR and submillimeter wavelengths. Studying the physical properties of obscured AGN and their host galaxies is crucial to shedding light on the early stages of a massive system lifetime. Aims. We aim to investigate the contribution of the interstellar medium (ISM) to the obscuration of quasars in a sample of distant highly star forming galaxies and to unveil their morphological and kinematics properties. Methods. We exploit Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 4 observations of the continuum (∼2.1mm) and high-J CO emission of a sample of six X-ray selected, far-IR detected galaxies hosting an obscured AGN at z spec > 2.5 in the 7 Ms Chandra Deep Field-South (CDF-S). We measured the masses and sizes of the dust and molecular gas by fitting the images, visibilities, and spectra, and we derived the gas density and column density on the basis of a uniform sphere geometry. Finally, we compared the measured column densities with those derived from the Chandra X-ray spectra. Results. We detected both the continuum and line emission for three sources for which we measured both the flux density and size. For the undetected sources, we derived an upper limit on the flux density from the root mean square (rms) of the images. We found that the detected galaxies are rich in gas and dust (molecular gas mass in the range <0.5 -2.7 × 10 10 M for α CO = 0.8 and up to ∼ 2 × 10 11 M for α CO = 6.5, and dust mass <0.9 -4.9 × 10 8 M ) and generally compact (gas major axis 2.1-3.0 kpc, dust major axis 1.4-2.7 kpc). The column densities associated with the ISM are on the order of 10 23−24 cm −2 , which is comparable with those derived from the X-ray spectra. For the detected sources we also derived dynamical masses in the range 0.8 -3.7 × 10 10 M . Conclusions. We conclude that the ISM of high redshift galaxies can substantially contribute to nuclear obscuration up to the Compton-thick (> 10 24 cm −2 ) regime. In addition, we found that all the detected sources show a velocity gradient reminding one rotating system, even though two of them show peculiar features in their morphology that can be associated with a chaotic, possibly merging, structure.

show abstract

Section: Source Sizecontrasting

confidence: 98%

Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

D’Amato

Gilli²,

Vignali³

et al. 2020

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…From the abundance of different SFR tracers (e.g. Hao et al 2011;Cortese et al 2012;Lee et al 2013;Boquien et al 2016;Casasola et al 2017), in this study, we are focusing on a reliable single MIR band SFR tracer (Calzetti et al 2010;Cluver et al 2017). Fig.…”

Section: Physical Properties and Dust Scaling Relationsmentioning

confidence: 99%

Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

Trčka

Baes

Camps

et al. 2020

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We compare the spectral energy distributions (SEDs) and inferred physical properties for simulated and observed galaxies at low redshift. We exploit UV-submillimetre mock fluxes of ∼ 7000 z=0 galaxies from the EAGLE suite of cosmological simulations, derived using the radiative transfer code skirt. We compare these to ∼ 800 observed galaxies in the UV-submillimetre range, from the DustPedia sample of nearby galaxies. To derive global properties, we apply the SED fitting code cigale consistently to both data sets, using the same set of ∼ 80 million models. The results of this comparison reveal overall agreement between the simulations and observations, both in the SEDs and in the derived physical properties, with a number of discrepancies. The optical and far-infrared regimes, and the scaling relations based upon the global emission, diffuse dust and stellar mass, show high levels of agreement. However, the mid-infrared fluxes of the EAGLE galaxies are overestimated while the far-UV domain is not attenuated enough, compared to the observations. We attribute these discrepancies to a combination of galaxy population differences between the samples, and limitations in the subgrid treatment of star-forming regions in the EAGLE-skirt post-processing recipe. Our findings show the importance of detailed radiative transfer calculations and consistent comparison, and provide suggestions for improved numerical models.

show abstract

“…We also selected these galaxies to be roughly representative of early-, mid-, and late-type barred spirals, with the basic properties of each galaxy given in Table 1. For two of them (NGC 1365 and M 83) a detailed analysis of the radial distribution of stars, gas, dust, and SFR is presented in Casasola et al (2017). NGC 1365 ( Fig.…”

Section: Galaxy Sample and Datamentioning

confidence: 99%

High-resolution, 3D radiative transfer modelling

Nersesian

Verstocken

Viaene

et al. 2020

A&A

View full text Add to dashboard Cite

Context. Dust in late-type galaxies in the local Universe is responsible for absorbing approximately one third of the energy emitted by stars. It is often assumed that dust heating is mainly attributable to the absorption of ultraviolet and optical photons emitted by the youngest (≤ 100 Myr) stars. Consequently, thermal re-emission by dust at far-infrared wavelengths is often linked to the starformation activity of a galaxy. However, several studies argue that the contribution to dust heating by much older stellar populations might be more significant than previously thought. Advances in radiation transfer simulations finally allow us to actually quantify the heating mechanisms of diffuse dust by the stellar radiation field. Aims. As one of the main goals in the DustPedia project, we have developed a framework to construct detailed 3D stellar and dust radiative transfer models for nearby galaxies. In this study, we analyse the contribution of the different stellar populations to the dust heating in four nearby face-on barred galaxies: NGC 1365, M 83, M 95, and M 100. We aim to quantify the fraction directly related to young stellar populations, both globally and on local scales, and to assess the influence of the bar on the heating fraction. Methods. From 2D images we derive the 3D distributions of stars and dust. To model the complex geometries, we used SKIRT, a state-of-the-art 3D Monte Carlo radiative transfer code designed to self-consistently simulate the absorption, scattering, and thermal re-emission by the dust for arbitrary 3D distributions. Results. We derive global attenuation laws for each galaxy and confirm that galaxies of high specific star-formation rate have shallower attenuation curves and weaker UV bumps. On average, 36.5% of the bolometric luminosity is absorbed by dust in our galaxy sample. We report a clear effect of the bar structure on the radial profiles of the dust-heating fraction by the young stellar populations, and the dust temperature. We find that the young stellar populations are the main contributors to the dust heating, donating, on average ∼ 59% of their luminosity to this purpose throughout the galaxy. This dust-heating fraction drops to ∼ 53% in the bar region and ∼ 38% in the bulge region where the old stars are the dominant contributors to the dust heating. We also find a strong link between the heating fraction by the young stellar populations and the specific star-formation rate.

show abstract

Radial distribution of dust, stars, gas, and star-formation rate in DustPedia face-on galaxies

Cited by 131 publications

References 189 publications

Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

Dust and gas content of high-redshift galaxies hosting obscured AGN in the Chandra Deep Field-South

Reproducing the Universe: a comparison between the EAGLE simulations and the nearby DustPedia galaxy sample

High-resolution, 3D radiative transfer modelling

Contact Info

Product

Resources

About