Modeling the infrared interstellar extinction

Wang, Shu; Li, Aigen; Jiang, Biwei

doi:10.1016/j.pss.2014.03.018

Cited by 42 publications

(43 citation statements)

References 59 publications

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“…The IR extinction law has been investigated by many authors. An overview of the observations was given by Wang et al (2014), while an overview of the corresponding models was given by Wang et al (2015). Their comparison suggests the presence of carbon grains with a radius of more than one micron in the medium.…”

Section: Discussionmentioning

confidence: 99%

Extinction law at a distance up to 25 kpc toward the Galactic poles

Gontcharov

2016

Astron. Lett.

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characteristics and properties of the Milky Way Galaxy, interstellar medium. Photometry from the Tycho-2, 2MASS, and WISE catalogues for clump and branch giants at a distance up to 25 kpc toward the Galactic poles has allowed the variations of various characteristics of the infrared interstellar extinction law with distance to be analyzed. The results obtained by the extinction law extrapolation method are consistent for different classes of stars and different characteristics as well as with previous studies. The conventional extinction law with a low infrared extinction is characteristic of only a thin layer no farther than 100 pc from the Galactic plane and of two thin layers near Z = −600 and +500 pc. Far from the Galactic plane, in the Galactic halo, the infrared extinction law is different: the extinction in the Ks, W 1, W 2, W 3, and W 4 bands is, respectively, 0.17, 0.16, 0.16, 0.07, and 0.03 of the extinction in the V band. The accuracy of these coefficients is 0.03. If the extinction law reflects primarily the grain size distribution, then the fraction of large dust grains far from the Galactic plane is greater than that in the circumsolar interstellar medium.

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Section: Discussionmentioning

confidence: 99%

Extinction law at a distance up to 25 kpc toward the Galactic poles

Gontcharov

2016

Astron. Lett.

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“…Our fitted slopes of G076.1807+00.0619 and G269.5205-01.2510, are over-plotted in Figure 3 and their equations are y = (3.2 ± 1.3)x + (2.8 ± 2.3) and y = (6.2 ± 5.0)x − (4.8 ± 11) respectively, where x and y are a color of W1−W2 and a magnitude of W1. In Figure 3, an extinction vector at R V = 5.5, typical value at both interstellar medium and dense molecular clouds in 3-8 µm (Weingartner & Draine 2001;Wang et al 2014), is also shown. G076.1807+00.0619 object shows a bluer (redder) color when the flux is increased (decreased) and the obtained slope is steeper than the 45 degree including fitting error.…”

Section: Color Variationmentioning

confidence: 96%

WISE Discovery of Mid-infrared Variability in Massive Young Stellar Objects

Uchiyama

Ichikawa²

2019

ApJ

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We systematically investigate the mid-infrared (MIR; λ > 3 µm) time variability of uniformly selected ∼ 800 massive young stellar objects (MYSOs) from the Red MSX Source (RMS) survey. Out of the 806 sources, we obtain reliable 9-year-long MIR magnitude variability data of 331 sources at the 3.4 µm (W1) and 4.6 µm (W2) bands by cross-matching the MYSO positions with ALLWISE and NEOWISE catalogs. After applying the variability selections using ALLWISE data, we identify 5 MIR-variable candidates. The light curves show various classes, with the periodic, plateau-like, and dipper features. Out of the obtained two color-magnitude diagram of W1 and W1−W2, one shows "bluer when brighter and redder when fainter" trends in variability, suggesting change in extinction or accretion rate. Finally, our results show that G335.9960−00.8532 (hereafter, G335) has a periodic light curve, with a ≈ 690-day cycle. Spectral energy density model fitting results indicate that G335 is a relatively evolved MYSO; thus, we may be witnessing the very early stages of a hyper-or ultra-compact H II region, a key source for understanding MYSO evolution.

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“…for silicate dust, and (Gao et al 2013(Gao et al , 2015Wang et al 2014). In addition, f cs will be 0.3 when the fraction of gas-phase carbon is 50%.…”

Section: Dust Modelsmentioning

confidence: 99%

Dust extinction towards the type Ia supernova 2012cu in NGC 4772

Gao

Zhao

Jian

et al. 2020

Planetary and Space Science

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Using photometric and spectroscopic data of Supernova (SN) 2012cu, a fairly reddened type Ia supernova, we derived its color excess curves and probed the dust extinction in its host galaxy, NGC 4772. In order to derive the extinction as a function of wavelength (i.e., A λ ), we model the color excess curves of SN 2012cu in terms of dust models consisting of silicate and carbonaceous (graphite or amorphous carbon) dust. The modeled extinction law towards SN 2012cu extends flatly to the far-ultraviolet (UV) bands, which is much flatter than those of the Milky Way and Magellanic Clouds, and the 2175Å feature is very weak or absent. The flatness of the modeled extinction curve in the UV bands suggests a "grey" extinction law of the active galactic nucleus in the vicinity of the SN 2012cu-Earth line of sight. Our results indicate that the sizes of the dust in the ISM towards SN 2012cu in NGC 4772 are larger than those of the Milky Way and the Large Magellanic Cloud, and much larger than that of the Small Magellanic Cloud. The best fitting gives an observed visual extinction towards SN 2012cu of A V ≈ 2.6 mag, a reddening * Corresponding author of E(B − V ) ≈ 1.0 mag, with a total-to-selective extinction ratio R V ≈ 2.7, consistent with previous results.

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Modeling the infrared interstellar extinction

Cited by 42 publications

References 59 publications

Extinction law at a distance up to 25 kpc toward the Galactic poles

Extinction law at a distance up to 25 kpc toward the Galactic poles

WISE Discovery of Mid-infrared Variability in Massive Young Stellar Objects

Dust extinction towards the type Ia supernova 2012cu in NGC 4772

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