Cold dust clumps in dynamically hot gas

Kim, S.; Kwon, E.; Madden, S.; Meixner, Margaret; Hony, S.; Panuzzo, P.; Sauvage, M.; Roman-Duval, Julia; Engelbracht, C. W.; Israel, F. P.; Misselt, K. A.; Okumura, K.; Li, A.; Bolatto, Alberto D.; Skibba, Ramin; Galliano, F.; Matsuura, M.; Bernard, J.-P.; Bot, Caroline; Galametz, M.; Hughes, Annie; Kawamura, Akiko; Onishi, Toshikazu; Paradis, D.; Poglitsch, A.; Reach, W. T.; Robitaille, Thomas; Rubio, M.; Tielens, A. G. G. M.

doi:10.1051/0004-6361/201014645

Cited by 10 publications

(4 citation statements)

References 33 publications

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“…The simulated dust traces the location of the bar; similarly, observed PAHs appear to be enhanced along the LMC stellar bar (Paradis et al 2009;Meixner et al 2010). Kim et al (2010) note that D is relatively uniform across the LMC, except in the vicinity of supershells, which are clustered around the bar (Williams et al 1999). Molecular clouds in the LMC are distinct and well spread throughout the disc (Fukui et al 2008), andKawamura et al (2009) establish the physical association between very young clusters in the LMC and GMCs.…”

Section: Spatial Distributions In the Lmcmentioning

confidence: 66%

Evolution of dust and molecular hydrogen in the Magellanic System

Yozin

Bekki

2014

Monthly Notices of the Royal Astronomical Society

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We investigate the evolution of the interstellar medium (ISM) in self-consistent, chemodynamical simulations of the Magellanic Clouds (MCs) during their recent (z < 0.3) past. An explicit modelling of dust and molecular hydrogen lifecycles enables us to compare our models against the observed properties of the ISM, including elemental depletion from the gas-phase. Combining this model with a tidal-dominated paradigm for the formation for the Magellanic Stream and Bridge, we reproduce the age-metallicity relations, long gas depletion timescales, and presently observed dust and molecular hydrogen masses of the MCs to within their respective uncertainties. We find that these models' enrichment depends sensitively on the processing of dust within the ISM and the dynamical influence of external tides/stellar bars. The ratio of characteristic dust destruction timescales in our SMC and LMC models, a governing parameter of our models' evolution, is consistent with estimates based on observed supernova (SN) rates. Our reference MC models tend to exhibit the disputed universal dust-to-metal ratio, which we argue stems from the adoption of high SNe II condensation efficiencies. Our models are the first to reproduce the one-tenth solar metallicity of the Stream/Leading Arm following tidal stripping of the SMC; the hypothesis that the LMC contributes a metal-rich filament to the Stream, as implied by recent kinematic and abundance analyses, is also appraised in this study.

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Section: Spatial Distributions In the Lmcmentioning

confidence: 66%

Evolution of dust and molecular hydrogen in the Magellanic System

Yozin

Bekki

2014

Monthly Notices of the Royal Astronomical Society

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“…It is now possible, with data from IRAS, Spitzer, and Herschel, to constrain the radial distributions of dust and stars within galaxies (Sauvage et al 1990;Zaritsky 1999;Muñoz-Mateos et al 2009;Mattsson & Andersen 2012), and to analyze the spatial distribution of dust, gas, and starlight in the MW (Paradis et al 2012), M31 (Smith et al 2012), M33 (Boquien et al 2011), and M83 (Foyle et al 2012), and other nearby galaxies (Aniano et al 2012;Galametz et al 2012). Others have added optical, Hα, and UV observations to constrain the evolution and environmental dependence of star formation in the LMC and SMC (Bell et al 2002;Harris & Zaritsky 2004Blair et al 2009;Lawton et al 2010), and clustering analyses have demonstrated the hierarchical formation of star clusters and dust clumps (Bonatto & Bica 2010;Kim et al 2010).…”

Section: Introductionmentioning

confidence: 99%

The Spatial Distribution of Dust and Stellar Emission of the Magellanic Clouds

Skibba¹,

Engelbracht²,

Aniano³

et al. 2012

ApJ

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We study the emission by dust and stars in the Large and Small Magellanic Clouds, a pair of lowmetallicity nearby galaxies, as traced by their spatially resolved spectral energy distributions (SEDs). This project combines Herschel Space Observatory PACS and SPIRE far-infrared photometry a with other data at infrared and optical wavelengths. We build maps of dust and stellar luminosity and mass of both Magellanic Clouds, and analyze the spatial distribution of dust/stellar luminosity and mass ratios. These ratios vary considerably throughout the galaxies, generally between the range 0.01 ≤ L dust /L * ≤ 0.6 and 10 −4 ≤ M dust /M * ≤ 4 × 10 −3 . We observe that the dust/stellar ratios depend on the interstellar medium (ISM) environment, such as the distance from currently or previously star-forming regions, and on the intensity of the interstellar radiation field (ISRF). In addition, we construct star formation rate (SFR) maps, and find that the SFR is correlated with the dust/stellar luminosity and dust temperature in both galaxies, demonstrating the relation between star formation, dust emission and heating, though these correlations exhibit substantial scatter.

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“…Over the past few decades, various methods of calculating SEDs have been reported. The latest SEDs for the LMC were introduced by Israel et al (2010), Kim et al (2010), andMeixner et al (2010). Galliano et al (2011) probed non-standard dust properties and extended submillimeter excess using the HSO observations.…”

Section: Resultsmentioning

confidence: 99%

Global spectral energy distributions of the Large Magellanic Cloud with interstellar dust

Kim

Kwon

Jeong

et al. 2013

Astrophys Space Sci

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The effects of dust on infrared emission vary among galaxies of different morphological types. We investigated integrated spectral energy distributions (SEDs) in infrared and submillimeter/millimeter emissions from the Large Magellanic Cloud (LMC) based on observations from the Herschel Space Observatory (HSO) and near-to mid-infrared observations from the Spitzer Space Telescope (SST). We also used IRAS and WMAP observations to constrain the SEDs and present the results of radiative transfer calculations using the spectrophotometric galaxy model. We explain the observations by using dust models with different grain size distributions in the interstellar medium of the LMC, noting that the LMC has undergone processes that differ from those in the Milky Way. We determined a spectral index and a normalisation factor in the range of −3.5 to −3.45 with grain radii in the range of 1 nm -300 nm for the silicate grain and 2 nm -1 µm for the graphite grain. The best fit to the observed SED was obtained with a spectral index of −3.47. The grain size distribution is described using a power law but with a break that is introduced below a b , where a larger exponent is used. Changing the graphite grain size distribution significantly changed the SED pattern within the observational uncertainties. Based on the SED fits to the observations from submillimeter wavelengths to infrared radiation from the LMC using GRASIL (Silva et al. 1998), we obtained a reasonable set of parameter values in chemical and geometric space together with the grain size distributions (Weingartner & Draine 2001) and a modified MRN model with the LMC extinction curve (Piovan et al. 2006a). For a given set of parameters including the disc scale height, synthesis of the starlight spectrum, optical depth, escape time scale, dust model, and star formation efficiency, the adopted dust-to-gas ratio for modeling the observed SEDs, ∼ 1/300 (from the literature) yields a reasonable fit to the observed SEDs and similar results with the metallicity of the LMC as those reported in Russell & Bessell (1989). The dust-to-gas ratios that are given as the metallicity caused the variation in the model fits.The difference mainly appears at the wavelength near 100 µm.

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Cold dust clumps in dynamically hot gas

Cited by 10 publications

References 33 publications

Evolution of dust and molecular hydrogen in the Magellanic System

Evolution of dust and molecular hydrogen in the Magellanic System

The Spatial Distribution of Dust and Stellar Emission of the Magellanic Clouds

Global spectral energy distributions of the Large Magellanic Cloud with interstellar dust

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