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• W4298131036 abstract "<i>Context. <i/>Ultraluminous infrared galaxies are merging systems characterized for containing large amounts of dust and emitting the bulk of their energy in the infrared. Dust affects several of the observed properties derived from optical and near-IR rest-frame data, such as the stellar morphology and the ionized gas distribution. Systematic analysis of the dust distribution in representative samples of ULIRGs are needed to investigate its two-dimensional structure, and to establish its impact in the derivation of fundamental properties such as star formation rates, effective radii, and dynamical masses.<i>Aims. <i/>We investigate the two-dimensional kpc-scale structure of the extinction in a representative sample of local ULIRGs using the H<i>α<i/>/H<i>β<i/> line ratio.<i>Methods. <i/>We use optical integral field spectroscopy obtained with the INTEGRAL instrument at the William Herschel Telescope. Complementary optical and near-IR high angular resolution HST images have also been used. Compared to classical optical long-slit analysis, our data provides information about the entire system, and not only in pre-selected orientations.<i>Results. <i/>The extinction exhibits a very complex and patchy structure in ULIRGs on kpc scales, from basically transparent regions to others deeply embedded in dust (<i>A<i/><sub>V<sub/> 0.0 to <i>A<i/><sub>V<sub/> 8.0 mag). Nuclear extinction covers a broad range in <i>A<i/><sub>V<sub/> from 0.4 to 7.7 mag , 69% of the nuclei having <i>A<i/><sub>V<sub/> <i>≥<i/> 2.0 mag. Extinction in the external regions is substantially lower than in the nuclei with 60% of the ULIRGs in the sample having median <i>A<i/><sub>V<sub/> of less than 2 mag for the entire galaxy. While post-coalescence nuclei tend to cluster around <i>A<i/><sub>V<sub/> values of 2 to 3 mag, pre-coalescence nuclei appear more homogeneously distributed over the entire 0.4 mag <i>≤<i/> <i>A<i/><sub>V<sub/> <i>≤<i/> 7.7 mag range. For the average extinction (<i>A<i/><sub>V<sub/> 2.0) derived for the ULIRGs of the sample, the ratio of the de-reddened to observed <i>SFR<i/> values is 6. The extinction-corrected, H<i>α<i/>-based <i>SFR<i/> ranges from 10 to 300 yr<sup>-1<sup/>. For only 27% of the cases the de-reddened <i>SFR<i/> is <20 yr<sup>-1<sup/>, whereas for the observed <i>SFR<i/> this percentage increases to 87%. The IR-based <i>SFR<i/> is always higher than the optical-based one, with differences ranging from about 2 to up to 30. The nuclear observed <i>SFR<i/> has an average contribution to the total one of 16% for the entire sample. Once corrected for extinction, the average value becomes 31%. Because of mostly extinction effects, the optical (<i>I<i/>-band) half-light radius in the sample galaxies is on average a factor 2.3 larger than the corresponding near-IR (<i>H<i/>-band) value." @default.
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• W4298131036 date "2009-07-22" @default.
• W4298131036 modified "2023-10-16" @default.
• W4298131036 title "Integral field optical spectroscopy of a representative sample of ULIRGs" @default.
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• W4298131036 doi "https://doi.org/10.1051/0004-6361/200912537" @default.
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