Inverse temperature dependence of the dust submillimeter spectral index

Dupac, X.; Bernard, J.-P.; Boudet, Nathalie; Giard, M.; Lamarre, J.-M.; Meny, C.; Pajot, F.; Ristorcelli, I.; Serra, G.; Stepnik, B.; Torre, J. P.

doi:10.1051/0004-6361:20030575

Cited by 259 publications

(400 citation statements)

References 39 publications

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“…Our results however do not rule out the hypothesis of a change in dust emissivity as a function of wavelength proposed in recent studies (e.g. Dupac et al 2003;Meny et al 2007). 6.…”

Section: Conclusion and Summarycontrasting

confidence: 99%

“…The submm excess could also be explained as a change in dust emissivity in lieu of the cold dust hypothesis. Models of Meny et al (2007) modify the dust optical properties to find an effective decrease in the submm emissivity index as the dust temperature increases as suggested by the observations of Dupac et al (2003). However, Shetty et al (2009) express caution in the inverse temperature -β interpretation, showing that flux uncertainties, especially in the Rayleigh-Jeans regime, can affect the results for the SED fits as far as temperature and emissivity are concerned.…”

Section: Refinement: Adding a Cold Dust Componentmentioning

confidence: 99%

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Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz¹,

Madden²,

Galliano³

et al. 2009

A&A

200

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Aims. We study the dust properties of four low metallicity galaxies by modelling their spectral energy distributions. This modelling enables us to constrain the dust properties such as the mass, the temperature or the composition to characterise the global ISM properties in dwarf galaxies. Methods. We present 870 μm images of four low metallicity galaxies (NGC 1705, Haro 11, Mrk 1089 and UM 311) observed with the Large APEX BOlometer CAmera (LABOCA) on the Atacama Pathfinder EXperiment (APEX) telescope. We modeled their spectral energy distributions combining the submm observations of LABOCA, 2MASS, IRAS, Spitzer photometric data, and the IRS data for Haro 11. Results. We found that the PAH mass abundance is very low in these galaxies, 5 to 50 times lower than the PAH mass fraction of our Galaxy. We also found that a significant mass of dust is revealed when using submm constraints compared to that measured with only mid-IR to far-IR observations extending only to 160 μm. For NGC 1705 and Haro 11, an excess in submillimeter wavelengths was detected when we used our standard dust SED model. We rerun our SED procedure adding a cold dust component (10 K) to better describe the high 870 μm flux derived from LABOCA observations, which significantly improves the fit. We found that at least 70% of the dust mass of these two galaxies can reside in a cold dust component. We also showed that the subsequent dust-to-gas mass ratios, considering HI and CO observations, can be strikingly high for Haro 11 in comparison with what is usually expected for these low-metallicity environments. Furthermore, we derived the star formation rate of our galaxies and compared them to the Schmidt law. Haro 11 falls anomalously far from the Schmidt relation. These results may suggest that a reservoir of hidden gas could be present in molecular form not traced by the current CO observations. While there can be a significant cold dust mass found in Haro 11, the SED peaks at exceptionally short wavelengths (36 μm), also highlighting the importance of the much warmer dust component heated by the massive star clusters in Haro 11. We also derived the total IR luminosities derived from our models and compared them with relations that derive this luminosity from Spitzer bands. We found that the Draine & Li (2007) formula compares well to our direct IR determinations.

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“…Our results however do not rule out the hypothesis of a change in dust emissivity as a function of wavelength proposed in recent studies (e.g. Dupac et al 2003;Meny et al 2007). 6.…”

Section: Conclusion and Summarycontrasting

confidence: 99%

Section: Refinement: Adding a Cold Dust Componentmentioning

confidence: 99%

Probing the dust properties of galaxies up to submillimetre wavelengths

Galametz¹,

Madden²,

Galliano³

et al. 2009

A&A

200

View full text Add to dashboard Cite

show abstract

“…There is growing evidence of an inverse relationship between the dust emissivity spectral index, β and the dust temperature, T d (Dupac et al 2003;Désert et al 2008;Paradis et al 2010;Veneziani et al 2010;Anderson et al 2012). We investigate this for the region associated with IRAS 20286+4105.…”

Section: Variation In Dust Emissivity Indexmentioning

confidence: 85%

Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

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A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 -B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be ∼ 175 M and 30 M . The mass-radius relation and the surface density of the clumps do not qualify them as massive star forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located toward the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.

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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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Inverse temperature dependence of the dust submillimeter spectral index

Cited by 259 publications

References 39 publications

Probing the dust properties of galaxies up to submillimetre wavelengths

Probing the dust properties of galaxies up to submillimetre wavelengths

Radio and infrared study of the star-forming region IRAS 20286+4105

Dusty star-forming galaxies at high redshift

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