The Araucaria Project: The Distance to the Small Magellanic Cloud From Near-Infrared Photometry of Rr Lyrae Variables

Szewczyk, O.; Pietrzyński, G.; Gieren, W.; Ciechanowska, A.; Bresolin, Fabio; Kudritzki, Rolf‐Peter

doi:10.1088/0004-6256/138/6/1661

Cited by 64 publications

(54 citation statements)

References 28 publications

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“…The Small and the Large Magellanic Clouds (SMC and LMC) are two of the nearest galaxies to ours (located at distances of 60 and 50 kpc respectively Deb & Singh 2010;Szewczyk et al 2009;Schaefer 2008;Szewczyk et al 2008). As such, they have been extensively observed in all wavelength regimes.…”

Section: Introductionmentioning

confidence: 57%

Submillimeter to centimeter excess emission from the Magellanic Clouds

Bot

Ysard

Paradis

et al. 2010

A&A

110

140

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Context. Dust emission at sub-millimeter to centimeter wavelengths is often simply the Rayleigh-Jeans tail of dust particles at thermal equilibrium and is used as a cold mass tracer in various environments, including nearby galaxies. However, well-sampled spectral energy distributions of the nearby, star-forming Magellanic Clouds have a pronounced (sub-)millimeter excess. Aims. This study attempts to confirm the existence of this millimeter excess above expected dust, free-free and synchrotron emission and to explore different possibilities for its origin. Methods. We model near-infrared to radio spectral energy distributions of the Magellanic Clouds with dust, free-free, and synchrotron emission. A millimeter excess emission is confirmed above these components and its spectral shape and intensity are analyzed in light of different scenarios: very cold dust, cosmic microwave background (CMB) fluctuations, a change of the dust spectral index and spinning dust emission. Results. We show that very cold dust or CMB fluctuations are very unlikely explanations for the observed excess in these two galaxies. The excess in the Large Magellanic Cloud can be satisfactorily explained either by a change of the spectral index related to intrinsic properties of amorphous grains, or by spinning dust emission. In the Small Magellanic Cloud, however, the excess is larger and the dust grain model including TLS/DCD effects cannot reproduce the observed emission in a simple way. A possible solution was achieved with spinning dust emission, but many assumptions on the physical state of the interstellar medium had to be made. Conclusions. Further studies, with higher resolution data from Planck and Herschel are needed to probe the origin of this observed submillimeter-centimeter excess more definitely. Our study shows that the different possible origins will be best distinguished where the excess is the highest, as is the case in the Small Magellanic Cloud.

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Section: Introductionmentioning

confidence: 57%

Submillimeter to centimeter excess emission from the Magellanic Clouds

Bot

Ysard

Paradis

et al. 2010

A&A

110

140

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“…Moreover, they have usually sampled either relatively small regions of space in our own Galaxy, or very large volumes in other galaxies (typically the inner few kpc). The nearby Magellanic Clouds (LMC: 50 kpc, Schaefer 2008; SMC: 61 kpc, Szewczyk et al 2009) provide an ideal opportunity to study objects with abundances significantly below solar, and at the same time study intermediate spatial scales. They are rich in interstellar gas and young, luminous stars, but carbon abundances are particularly low.…”

Section: Introductionmentioning

confidence: 99%

C⁺emission from the Magellanic Clouds

Israel

Maloney

2011

A&A

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Context. We study the λ 158 μm [C II] fine-structure line emission from star-forming regions as a function of metallicity. Aims. We have measured and mapped the [C II] emission from the very bright HII region complexes N 11 in the LMC and N 66 in the SMC; as well as the SMC H II regions N 25, N 27, N 83/N 84, and N 88 with the FIFI instrument on the Kuiper Airborne Observatory. Methods. In both LMC and SMC, the ratio of [C II] line to CO line and to the far-infrared continuum emission is much higher than seen almost anywhere else, including Milky Way star-forming regions, and whole galaxies. Results. In the low metallicity, low dust-abundance environment of the LMC and the SMC UV mean free path lengths are much greater than those in the higher-metallicity Milky Way. The increased photoelectric heating efficiencies cause significantly greater relative [C II] line emission strengths. At the same time, similar decreases in PAH abundances have the opposite effect by diminishing photoelectric heating rates. Consequently, in low-metallicity environments relative [C II] strengths are high but exhibit little further dependence on actual metallicity. Relative [C II] strengths are slightly higher in the LMC than in the SMC which has both lower dust and lower PAH abundances.

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“…Schaefer 2008; 61 kpc, Szewczyk et al 2009) permits detailed studies of resolved ISM clouds and their relation to stellar populations on global scales, in an unambiguous manner, and as a controlled function of environment. Their sub-solar metallicities (Z LMC 0.5 × Z , Z SMC 0.2 × Z ; Dufour et al 1982;Bernard et al 2006) permit investigations on how processes governing galaxy evolution depend on metallicity.…”

Section: Introductionmentioning

confidence: 99%

HERschelInventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust

Meixner

Galliano

Hony

et al. 2010

A&A

111

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The HERschel Inventory of The Agents of Galaxy Evolution (HERITAGE) of the Magellanic Clouds will use dust emission to investigate the life cycle of matter in both the Large and Small Magellanic Clouds (LMC and SMC). Using the Herschel Space Observatory's PACS and SPIRE photometry cameras, we imaged a 2 • × 8 • strip through the LMC, at a position angle of ∼22.5 • as part of the science demonstration phase of the Herschel mission. We present the data in all 5 Herschel bands: PACS 100 and 160 μm and SPIRE 250, 350 and 500 μm. We present two dust models that both adequately fit the spectral energy distribution for the entire strip and both reveal that the SPIRE 500 μm emission is in excess of the models by ∼6 to 17%. The SPIRE emission follows the distribution of the dust mass, which is derived from the model. The PAH-to-dust mass ( f PAH ) image of the strip reveals a possible enhancement in the LMC bar in agreement with previous work. We compare the gas mass distribution derived from the HI 21 cm and CO J = 1−0 line emission maps to the dust mass map from the models and derive gas-to-dust mass ratios (GDRs). The dust model, which uses the standard graphite and silicate optical properties for Galactic dust, has a very low GDR = 65 +15 −18making it an unrealistic dust model for the LMC. Our second dust model, which uses amorphous carbon instead of graphite, has a flatter emissivity index in the submillimeter and results in a GDR = 287 +25 −42 that is more consistent with a GDR inferred from extinction.

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The Araucaria Project: The Distance to the Small Magellanic Cloud From Near-Infrared Photometry of Rr Lyrae Variables

Cited by 64 publications

References 28 publications

Submillimeter to centimeter excess emission from the Magellanic Clouds

Submillimeter to centimeter excess emission from the Magellanic Clouds

C⁺emission from the Magellanic Clouds

HERschelInventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust

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The Araucaria Project: The Distance to the Small Magellanic Cloud From Near-Infrared Photometry of Rr Lyrae Variables

Cited by 64 publications

References 28 publications

Submillimeter to centimeter excess emission from the Magellanic Clouds

Submillimeter to centimeter excess emission from the Magellanic Clouds

C+emission from the Magellanic Clouds

HERschelInventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust

Contact Info

Product

Resources

About

C⁺emission from the Magellanic Clouds