Variation in the dust emissivity index across M 33 with<i>Herschel</i>and<i>Spitzer</i>(HerM 33es)

Tabatabaei, F. S.; Braine, J.; Xilouris, E. M.; Krämer, C.; Boquien, M.; Combes, F.; Henkel, C.; Relaño, M.; Verley, S.; Gratier, P.; Israel, F. P.; Wiedner, Martina C.; Röllig, M.; Schüster, K.; Werf, P. van der

doi:10.1051/0004-6361/201321441

Cited by 69 publications

(98 citation statements)

References 73 publications

(78 reference statements)

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“…The spectral emissivity index, β, is often assumed to be 1.5 (and is found to usually range between 1-2 in starburst galaxies Hildebrand, 1983;Dunne & Eales, 2001;Chapin et al, 2011). Note that several works on nearby molecular clouds and dusty regions in nearby galaxies debate whether or not β also has temperature dependence, with laboratory experiments suggesting an anti-correlation (Lisenfeld et al, 2000;Dupac et al, 2003;Paradis et al, 2009;Shetty et al, 2009a,b;Veneziani et al, 2010;Bracco et al, 2011;Tabatabaei et al, 2013), although that has little impact on the implied SED fit for unresolved distant DSFGs where the effective temperature is only representative of the aggrigate dust temperatures contained within. Note that some works assume that DSFGs galaxies can be approximated as optically thin modified blackbodies, such that the (1−e −τ(ν) ) term reduces to ν β .…”

Section: Direct Modified Blackbody Sed Modelingmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Section: Direct Modified Blackbody Sed Modelingmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…A decreasing spectral index for the absorption cross section with radius, and thus possible variations in the dust properties along the disk, has been reported for MBB fits to M 31 (Smith et al 2012a) and M 33 (Tabatabaei et al 2014). Though this change in properties might affect the dust gradients, we did not try fits with varying β, as the dust mass determination would also need a knowledge of the unknown variations of the absorption cross section normalization with the environment.…”

Section: Dust Massmentioning

confidence: 99%

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

Casasola

Cassarà

Bianchi

et al. 2017

A&A

131

140

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Aims. The purpose of this work is the characterization of the radial distribution of dust, stars, gas, and star-formation rate (SFR) in a sub-sample of 18 face-on spiral galaxies extracted from the DustPedia sample. Methods. This study is performed by exploiting the multi-wavelength, from ultraviolet (UV) to sub-millimeter bands, DustPedia database, in addition to molecular ( 12 CO) and atomic (Hi) gas maps and metallicity abundance information available in the literature. We fitted the surface brightness profiles of the tracers of dust and stars, the mass surface density profiles of dust, stars, molecular gas, and total gas, and the SFR surface density profiles with an exponential curve and derived their scale-lengths. We also developed a method to solve for the CO-to-H 2 conversion factor (α CO ) per galaxy by using dust and gas mass profiles. Results. Although each galaxy has its own peculiar behaviour, we identified a common trend of the exponential scale-lengths vs. wavelength. On average, the scale-lengths normalized to the B-band 25 mag/arcsec 2 radius decrease from UV to 70 µm, from 0.4 to 0.2, and then increase back up to ∼0.3 at 500 microns. The main result is that, on average, the dust mass surface density scale-length is about 1.8 times the stellar one derived from IRAC data and the 3.6 µm surface brightness, and close to that in the UV. We found a mild dependence of the scale-lengths on the Hubble stage T: the scale-lengths of the Herschel bands and the 3.6 µm scale-length tend to increase from earlier to later types, the scale-length at 70 µm tends to be smaller than that at longer sub-mm wavelength with ratios between longer sub-mm wavelengths and 70 µm that decrease with increasing T. The scale-length ratio of SFR and stars shows a weak increasing trend towards later types. Our α CO determinations are in the range (0.3 − 9) M pc −2 (K km s −1 ) −1 , almost invariant by using a fixed dust-to-gas ratio mass (DGR) or a DGR depending on metallicity gradient.

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“…We, therefore, argue that the assumed relative dust-to-stellar scale height h z,d /h z, = 0.5 provides a good representation of the true vertical distribution of stars and dust in M 51. We do need to be cautious regarding uncertainties on the assumed dust model parameters, i.e., deviations from the assumed dust opacity κ, and its variation with wavelength (e.g., Tabatabaei et al 2014;Gordon et al 2014), which will reflect in a similar uncertainty on the dust mass determination, FUV attenuation, and dust emission in IR/submm wavebands.…”

Section: Appendix A: the Effect Of Model Degeneraciesmentioning

confidence: 99%

High-resolution, 3D radiative transfer modeling

Looze

Fritz

Baes

et al. 2014

A&A

100

114

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Context. Dust reprocesses about half of the stellar radiation in galaxies. The thermal re-emission by dust of absorbed energy is considered to be driven merely by young stars so is often applied to tracing the star formation rate in galaxies. Recent studies have argued that the old stellar population might be responsible for a non-negligible fraction of the radiative dust heating. Aims. In this work, we aim to analyze the contribution of young ( < ∼ 100 Myr) and old (∼10 Gyr) stellar populations to radiative dust heating processes in the nearby grand-design spiral galaxy M 51 using radiative transfer modeling. High-resolution 3D radiative transfer (RT) models are required to describe the complex morphologies of asymmetric spiral arms and clumpy star-forming regions and to model the propagation of light through a dusty medium. Methods. In this paper, we present a new technique developed to model the radiative transfer effects in nearby face-on galaxies. We construct a high-resolution 3D radiative transfer model with the Monte-Carlo code SKIRT to account for the absorption, scattering, and non-local thermal equilibrium (NLTE) emission of dust in M 51. The 3D distribution of stars is derived from the 2D morphology observed in the IRAC 3.6 µm, GALEX FUV, Hα, and MIPS 24 µm wavebands, assuming an exponential vertical distribution with an appropriate scale height. The dust geometry is constrained through the far-ultraviolet (FUV) attenuation, which is derived from the observed total-infrared-to-far-ultraviolet luminosity ratio. The stellar luminosity, star formation rate, and dust mass have been scaled to reproduce the observed stellar spectral energy distribution (SED), FUV attenuation, and infrared SED. Results. The dust emission derived from RT calculations is consistent with far-infrared and submillimeter observations of M 51, implying that the absorbed stellar energy is balanced by the thermal re-emission of dust. The young stars provide 63% of the energy for heating the dust responsible for the total infrared emission (8−1000 µm), while 37% of the dust emission is governed through heating by the evolved stellar population. In individual wavebands, the contribution from young stars to the dust heating dominates at all infrared wavebands but gradually decreases towards longer infrared and submillimeter wavebands for which the old stellar population becomes a non-negligible source of heating. Upon extrapolation of the results for M 51, we present prescriptions for estimating the contribution of young stars to the global dust heating based on a tight correlation between the dust heating fraction and specific star formation rate.

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Variation in the dust emissivity index across M 33 withHerschelandSpitzer(HerM 33es)

Cited by 69 publications

References 73 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

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

High-resolution, 3D radiative transfer modeling

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