Characterizing Dust Attenuation in Local Star-forming Galaxies: Near-infrared Reddening and Normalization

Battisti, Andrew; Calzetti, Daniela; Chary, R.-R.

doi:10.3847/1538-4357/aa6fb2

Cited by 39 publications

(60 citation statements)

References 73 publications

(165 reference statements)

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“…For the purpose of this analysis, we assume a foreground-like dust component is dominating the attenuation, which is consistent with the linear relationship between these quantities and provides us with a straightforward manner to derive the effective attenuation curve. However, we stress that more complex geometries are likely to occur and may account for some of the scatter in the observed relationship (see Battisti et al 2016Battisti et al , 2017, for more discussion).…”

Section: Galaxy Templatesmentioning

confidence: 99%

“…To empirically determine our attenuation curves, we follow the same methodology as previously employed in Battisti et al (2016Battisti et al ( , 2017. This requires comparing the SEDs of galaxies with differing amounts of dust attenuation while also accounting for intrinsic differences between the stellar populations among our sample, which can lead to significant SED variation independent of the total level of dust attenuation.…”

Section: Galaxy Templatesmentioning

confidence: 99%

“…In Battisti et al (2017), we cross-matched our sample with NIR sources in the United Kingdom Infrared Telescope (UKIRT) Infrared Deep Sky Survey (UKIDSS; Hewett et al 2006) and the Two Micron All-sky Survey (2MASS; Skrutskie et al 2006). The former survey is deeper than the latter but only encompasses a fraction of the SDSS footprint, thus using both provides us with good statistics for both faint (common) and bright (rare) galaxies.…”

Section: Sample Selectionmentioning

confidence: 99%

“…We select galaxies within a window of D 4000 0.2 n D = , which is centered on the mean value of 1.2 and 1.23 for the UV-optical and UV-NIR samples, respectively. For the NIR analysis, we also impose a restriction on the stellar mass range of M M 9.1 log 9.9 * < <  [ ( )] to mitigate the variation in the NIR due to the old, low-mass stellar populations (Battisti et al 2017), for which D 4000 n is insufficient to constrain because it is primarily linked to intermediate mass stars. The logic behind the chosen D 4000 n and M * windows is to retain the largest fraction of the galaxy sample while also reducing the influence of stellar population age on the derived attenuation curve.…”

Section: Galaxy Templatesmentioning

confidence: 99%

“…The goal of this study is to extend on the work of our previous studies (Battisti et al 2016(Battisti et al , 2017 by quantifying the influence that inclination has on the shape and normalization on dust attenuation curves, as well as its role on the strength of the 2175Å feature, using a sample of ∼10,000 local SFGs. The benefit of this sample is that the amount of dust attenuation for each galaxy can be robustly inferred from the Balmer decrement, whereas most previous studies have employed SED modeling techniques that are dependent on the assumed stellar population and therefore subject to more uncertainty and potential biases.…”

Section: Introductionmentioning

confidence: 99%

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Characterizing Dust Attenuation in Local Star-forming Galaxies: Inclination Effects and the 2175 Å Feature

Battisti

Calzetti

Chary

2017

ApJ

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We characterize the influence that inclination has on the shape and normalization in average dust attenuation curves derived from a sample of ∼10,000 local star-forming galaxies. To do this, we utilize aperture-matched multiwavelength data from the Galaxy Evolution Explorer, the Sloan Digital Sky Survey, the United Kingdom Infrared Telescope, and the Two Micron All-sky Survey. We separate our sample into groups according to axial ratio (b/a) and obtain an estimate of their average total-to-selective attenuation k l ( ). The attenuation curves are found to be shallower at UV wavelengths with increasing inclination, whereas the shape at longer wavelengths remains unchanged. The highest inclination subpopulation (b a 0.42 < ) exhibits an NUV excess in its average selective attenuation, which, if interpreted as a 2175Å feature, is best fit with a bump strength of 17%-26% of the MW value. No excess is apparent in the average attenuation curve of lower inclination galaxies. The differential reddening between the stellar continuum and ionized gas is found to decrease with increasing inclination. We find that higher inclination galaxies have slightly higher values of R V , although this is poorly constrained given the uncertainties. We outline possible explanations for these trends within a two component dust model (dense cloud +diffuse dust) and find that they can be naturally explained if carriers of the 2175Å feature are preferentially destroyed in star-forming regions (UV-bright regions).

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Section: Galaxy Templatesmentioning

confidence: 99%

Section: Galaxy Templatesmentioning

confidence: 99%

Section: Sample Selectionmentioning

confidence: 99%

Section: Galaxy Templatesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Characterizing Dust Attenuation in Local Star-forming Galaxies: Inclination Effects and the 2175 Å Feature

Battisti

Calzetti

Chary

2017

ApJ

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Investigation of dust attenuation and star formation activity in galaxies hosting GRBs

Corre

Buat

Basa

et al. 2018

A&A

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Context. The gamma-ray bursts hosts (GRBHs) are excellent targets to study the extinction properties of dust and its effects on the global emission of distant galaxies. The dust extinction curve is measured along the GRB afterglow line of sight and the analysis of the spectral energy distribution (SED) of the host galaxy gives access to the global dust attenuation of the stellar light. Aims. In this pilot study we gather information on dust extinction in GRBHs to compare the properties of the extinction curve to those of the dust obscuration affecting the total stellar light of the host galaxy. Assuming the extinction curve to be representative of the dust properties, we aim to investigate which dust-stars geometries and local dust distribution in the inter stellar medium (ISM) can reproduce the observed attenuation curve. Methods. We selected a sample of 30 GRBs for which the extinction curve along the GRB afterglow line-of-sight (l.o.s) is measured in the rest-frame ultraviolet (UV) up to optical and we analysed the properties of the extinction curve as a function of the host galaxy properties. From these 30 GRBs, we selected seven GRBHs with a good rest-frame UV to near infra-red (NIR) spectral coverage for the host. The attenuation curve was derived by fitting the SEDs of the GRBH sample with the CIGALE SED fitting code. Different star formation histories (SFH) were studied to recover the star formation rates (SFR) derived using Hα luminosities. Implications for the dust-stars geometries in the ISM are inferred by a comparison with radiative transfer simulations. Results. The most extinguished GRBs are preferentially found in the more massive hosts and the UV bump is preferentially found in the most extinguished GRB l.o.s. Five out of seven hosts are best fitted with a recent burst of star formation, leading to lower stellar mass estimates than previously found. The average attenuation in the host galaxies is about 70% of the amount of extinction along the GRB l.o.s. We find a great variety in the derived attenuation curves of GRBHs, the UV slope can be similar, flatter or even steeper than the extinction curve slope. Half of the attenuation curves are consistent with the Calzetti attenuation law and there is evidence of a UV bump in only one GRBH. We find that the flatter (steeper) attenuation curves are found in galaxies with the highest (lowest) SFR and stellar masses. The comparison of our results with radiative transfer simulations leads to a uniform distribution of dust and stars in a very clumpy ISM for half the GRBHs and various dust-stars geometries for the second half of the sample.

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Dust attenuation and Hα emission in a sample of galaxies observed with Herschel at 0.6 < z < 1.6

Buat

Boquien

Małek

et al. 2018

A&A

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Context. Dust attenuation shapes the spectral energy distribution of galaxies. It is particularly true for dusty galaxies in which stars experience a heavy attenuation. The combination of UV to IR photometry with the spectroscopic measurement of the Hα recombination line helps to quantify dust attenuation of the whole stellar population and its wavelength dependence. Aims. We want to derive the shape of the global attenuation curve and the amount of obscuration affecting young stars or nebular emission and the bulk of the stellar emission in a representative sample of galaxies selected in IR. We will compare our results to the commonly used recipes of Calzetti et al. and Charlot and Fall, and to predictions of radiative transfer models. Methods. We selected an IR complete sample of galaxies in the COSMOS 3D-HST CANDELS field detected with the Herschel satellite with a signal to noise ratio larger than five. Optical to NIR photometry is available as well as NIR spectroscopy for each source. We reduced the sample to the redshift range 0.6 < z < 1.6 to include the Hα line in the G141 grism spectra. We have used a new version of the CIGALE code to fit simultaneously the continuum and Hα line emission of the 34 selected galaxies. Results. Using flexible attenuation laws with free parameters, we are able to measure the shape of the attenuation curve for each galaxy as well as the amount of attenuation of each stellar population, the former being in general steeper than the starburst law in the UV-optical with a large variation of the slope among galaxies. The attenuation of young stars or nebular continuum is found on average about twice the attenuation affecting older stars, again with a large variation. Our model with power-laws, based on a modification of the Charlot and Fall recipe, gives results in better agreement with the radiative transfer models than the global modification of the slope of the Calzetti law.

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Characterizing Dust Attenuation in Local Star-forming Galaxies: Near-infrared Reddening and Normalization

Cited by 39 publications

References 73 publications

Characterizing Dust Attenuation in Local Star-forming Galaxies: Inclination Effects and the 2175 Å Feature

Characterizing Dust Attenuation in Local Star-forming Galaxies: Inclination Effects and the 2175 Å Feature

Investigation of dust attenuation and star formation activity in galaxies hosting GRBs

Dust attenuation and Hα emission in a sample of galaxies observed with Herschel at 0.6 < z < 1.6

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