Detection of Ultraviolet Halos Around Highly Inclined Galaxies

Hodges-Kluck, Edmund; Bregman, Joel N.

doi:10.1088/0004-637x/789/2/131

Cited by 54 publications

(63 citation statements)

References 70 publications

(96 reference statements)

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“…A1 become visible. From an inspection of the intrinsic stellar emission edge-on map, we notice that the increasing visibility of the bulge is not due to the presence of dust but it is an intrinsic feature of the galaxy stellar emission; (vi) although one sees light in the UV coming from the galaxy halo, this is not as prominent as seen in nearby edge-on galaxies in the local universe where the UV halo emission is comparable to or even exceeds the direct light seen from the disc (Seon et al 2014, Hodges-Kluck & Bregman 2014.…”

Section: Predicted Surface Brightness Distributions Of Stellar Lightmentioning

confidence: 80%

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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Section: Predicted Surface Brightness Distributions Of Stellar Lightmentioning

confidence: 80%

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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“…Hodges-Kluck & Bregman (2014) found a correlation between the UV halo luminosity and the star formation rate. A nearly linear correlation between the extraplanar PAH flux and the star formation activity in the disk was also found (McCormick et al 2013).…”

Section: Discussionmentioning

confidence: 91%

“…On the other hand, Hodges-Kluck & Bregman (2014) claimed that the the halo colors and luminosities are consistent with the SMC-type dust (lacking a 2175Å UV "absorption" bump), using a simple reflection nebula model. However, the SED of the scattered flux in an optically thin environment depends only on the wavelength dependence of the scattering efficiency of the grains.…”

Section: Discussionmentioning

confidence: 98%

“…The discovery of the UV halos due to the diffuse dust existing above the galactic plane of NGC 891 was first reported in Seon & Witt (2012a). Hodges-Kluck & Bregman (2014) describe the discovery of the UV halos around many galaxies, including NGC 891. In this Letter, we use a radiative transfer model to study the content of the extended UV emission in NGC 891.…”

Section: Introductionmentioning

confidence: 99%

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Diffuse Extraplanar Dust in NGC 891

Seon

Witt

Shinn

et al. 2014

ApJ

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We report the detection of vertically extended far-ultraviolet (FUV) and near-UV emissions in an edge-on spiral galaxy NGC 891, which we interpret as being due to dust-scattered starlight. Three-dimensional radiative transfer models are used to investigate the content of the extraplanar dust that is required to explain the UV emission. The UV halos are well reproduced by a radiative transfer model with two exponential dust disks, one with a scaleheight of ≈ 0.2 − 0.25 kpc and the other with a scaleheight of ≈ 1.2 − 2.0 kpc. The central face-on optical depth of the geometrically thick disk is found to be τ thick B ≈ 0.3 − 0.5 at B-band. The results indicate that the dust mass at |z| > 2 kpc is ≈ 3 − 5% of the total dust mass, which accord well with the recent Herschel sub-millimeter observation. Our results, together with the recent discovery of the UV halos in other edge-on galaxies, suggest the widespread existence of the geometrically thick dust layer above the galactic plane in spirals.

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“…Alternatively, it could be diffuse scattered light produced by a radially extended PSF (Sandin 2014) or scattered emission from a vertically extended dust distribution (see e.g. Hodges-Kluck & Bregman 2014;Shinn & Seon 2015;). …”

Section: Comparing the Observed And Simulated Imagesmentioning

confidence: 99%

HERschelObservations of Edge-on Spirals (HEROES)

Mosenkov

Allaert

Baes

et al. 2016

A&A

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We investigate the dust energy balance for the edge-on galaxy IC 2531, one of the seven galaxies in the HEROES sample. We perform a state-of-the-art radiative transfer modelling based, for the first time, on a set of optical and near-infrared galaxy images. We show that by taking into account near-infrared imaging in the modelling significantly improves the constraints on the retrieved parameters of the dust content. We confirm the result from previous studies that including a young stellar population in the modelling is important to explain the observed stellar energy distribution. However, the discrepancy between the observed and modelled thermal emission at far-infrared wavelengths, the so-called dust energy balance problem, is still present: the model underestimates the observed fluxes by a factor of about two. We compare two different dust models, and find that dust parameters, and thus the spectral energy distribution in the infrared domain, are sensitive to the adopted dust model. In general, the THEMIS model reproduces the observed emission in the infrared wavelength domain better than the popular BARE-GR-S model. Our study of IC 2531 is a pilot case for detailed and uniform radiative transfer modelling of the entire HEROES sample, which will shed more light on the strength and origins of the dust energy balance problem.

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Detection of Ultraviolet Halos Around Highly Inclined Galaxies

Cited by 54 publications

References 70 publications

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

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

Diffuse Extraplanar Dust in NGC 891

HERschelObservations of Edge-on Spirals (HEROES)

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