Investigations of dust heating in M81, M83 and NGC 2403 with the Herschel Space Observatory

Bendo, G. J.; Boselli, A.; Dariush, A.; Pohlen, M.; Roussel, H.; Sauvage, M.; Smith, M.; Wilson, C. D.; Baes, M.; Cooray, Asantha; Clements, D. L.; Cortese, Luca; Foyle, K.; Galametz, M.; Gomez, Haley Louise; Lebouteiller, V.; Lu, N.; Madden, S.; Mentuch, Erin; O’Halloran, B.; Page, M. J.; Rémy, Aurélie; Schulz, B.; Spinoglio, L.

doi:10.1111/j.1365-2966.2011.19735.x

Cited by 158 publications

(259 citation statements)

References 93 publications

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“…We note in Figure 3 that the SFR 24 /SFR H ratio is less discrepant for massive IR-faint QGs candidates than less massive ones, which contradicts the expectations if old stellar populations are primarily responsible for the FIR emission. However, the temperature gradient is needed to determine the integrated dust SED shape (Bendo et al 2012). The lack of its direct measurement in our QG sample restricts us from making further remarks on the massdependent trend of SFR 24 /SFR H for IR-faint QGs.…”

Section: Estimations Of Ir Luminosities and Sfrsmentioning

confidence: 99%

“…longer than 160 μm (Bendo et al 2012; see also Bell 2003;Salim et al 2009;Fumagalli et al 2014), which are most relevant for the Herschel SPIRE bands. We note in Figure 3 that the SFR 24 /SFR H ratio is less discrepant for massive IR-faint QGs candidates than less massive ones, which contradicts the expectations if old stellar populations are primarily responsible for the FIR emission.…”

Section: Estimations Of Ir Luminosities and Sfrsmentioning

confidence: 99%

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CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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We performed a comprehensive stacking analysis on ∼14,200 quiescent galaxy (QG) candidates at z=0-3 across mid-, far-infrared (MIR and FIR), and radio wavelengths. Identified via their rest-frame NUV−r and r−J colors, the QG candidates (M M 10 9.8 12.2 - =  ) have drastically different IR and radio properties depending on their 24 μm emission strength. The fraction of QG candidates with strong 24 μm emission (equivalent to inferred star formation rates SFR M yr 100, hereafter "IR-bright") increases with redshift and peaks at 15%, and their stacked MIPS 24 μm, Herschel (PACS and SPIRE) and VLA emissions are consistent with being starforming galaxies (SFGs). In contrast, the majority of QG candidates are faint or undetected at 24 μm individually (i.e., SFR 24 <100 M e yr −1 , hereafter "IR-faint"). Their low dust-obscured SFRs derived from Herschel stacking (SFR H  3, 15, 50 M e yr −1 out to z∼1, 2, 3) are >2.5-12.5×lower than compared to SFGs. This is consistent with the quiescence, as expected from their low unobscured SFRs, as inferred from modeling their ultraviolet-to-NIR photometry. The discrepancy between the L IR derived from stacking Herschel and 24 μm indicates that IRfaint QGs have dust SEDs that are different from those of SFGs. For the most massive (M M 10 11    ) IR-faint QGs at z<1.5, the stacked 1.4 GHz emission is in excess of that expected from other SFR indicators, suggesting a widespread presence of low-luminosity active galactic nuclei. Our results reaffirm the existence of a significant population of QGs out to z=3, thus corroborating the need to quench star formation in galaxies at early epochs.

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Section: Estimations Of Ir Luminosities and Sfrsmentioning

confidence: 99%

Section: Estimations Of Ir Luminosities and Sfrsmentioning

confidence: 99%

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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“…Many authors have tried to address this question, mainly relying on sim- ple geometrical comparisons between the surface brightness distributions at different wavelengths (e.g. Boquien et al 2011, Bendo et al 2012. Such comparisons make the implicit assumption that the stellar emissivity within the resolution element of the telescope dominates the heating of the dust which is visible in the same telescope beam.…”

Section: Calculation Of the Dust Emission Fraction Powered By Young Amentioning

confidence: 99%

“…Indeed, farinfrared(FIR)/submm observations of spiral galaxies show that most of the dust emission luminosity is emitted longwards of 100 micron (see e.g. Sodroski et al 1997, Odenwald et al 1998, 2012, Bendo et al 2012) through grains situated in the diffuse ISM, which are generally located at very considerable distances from the stars heating the dust. In addition, infrared radiation shortwards of 100 µm is also known to have a significant contribution from small grains out of equilibrium with the radiation fields of low energy densities, the so-called stochastically heated grains.…”

Section: Calculation Of Dust Emission Using Dart-raymentioning

confidence: 99%

Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with dart-ray

Natale¹,

Popescu²,

Tuffs³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We describe the calculation of the stochastically heated dust emission using the 3D ray-tracing dust radiative transfer code DART-Ray, which is designed to solve the dust radiative transfer problem for galaxies with arbitrary geometries. In order to reduce the time required to derive the non-equilibrium dust emission spectra from each volume element within a model, we implemented an adaptive SED library approach, which we tested for the case of axisymmetric galaxy geometries. To show the capabilities of the code, we applied DART-Ray to a highresolution N-body+SPH galaxy simulation to predict the appearance of the simulated galaxy at a set of wavelengths from the UV to the sub-mm. We analyse the results to determine the effect of dust on the observed radial and vertical profiles of the stellar emission as well as on the attenuation and scattering of light from the constituent stellar populations. We also quantify the proportion of dust re-radiated stellar light powered by young and old stellar populations, both bolometrically and as a function of infrared wavelength.

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“…This poor spatial resolution limits a detailed study of the dust medium to the most nearby galaxies only (e.g. Meixner et al 2010;Bendo et al 2010Bendo et al , 2012Xilouris et al 2012;Foyle et al 2012;De Looze et al 2012b;Fritz et al 2012;Smith et al 2012a;Galametz et al 2012). Moreover, several authors have demonstrated that even estimating total dust masses from global fluxes induces an error due to resolution effects (Galliano et al 2011;Galametz et al 2012).…”

Section: Introductionmentioning

confidence: 99%

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

Geyter

Baes

Fritz

et al. 2013

A&A

Self Cite

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We present FitSKIRT, a method to efficiently fit radiative transfer models to UV/optical images of dusty galaxies. These images have the advantage that they have better spatial resolution compared to FIR/submm data. FitSKIRT uses the GAlib genetic algorithm library to optimize the output of the SKIRT Monte Carlo radiative transfer code. Genetic algorithms prove to be a valuable tool in handling the multi-dimensional search space as well as the noise induced by the random nature of the Monte Carlo radiative transfer code. FitSKIRT is tested on artificial images of a simulated edge-on spiral galaxy, where we gradually increase the number of fitted parameters. We find that we can recover all model parameters, even if all 11 model parameters are left unconstrained. Finally, we apply the FitSKIRT code to a V-band image of the edge-on spiral galaxy NGC 4013. This galaxy has been modeled previously by other authors using different combinations of radiative transfer codes and optimization methods. Given the different models and techniques and the complexity and degeneracies in the parameter space, we find reasonable agreement between the different models. We conclude that the FitSKIRT method allows comparison between different models and geometries in a quantitative manner and minimizes the need of human intervention and biasing. The high level of automation makes it an ideal tool to use on larger sets of observed data.

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Investigations of dust heating in M81, M83 and NGC 2403 with the Herschel Space Observatory

Cited by 158 publications

References 93 publications

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Predicting the stellar and non-equilibrium dust emission spectra of high-resolution simulated galaxies with dart-ray

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

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