English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We study the wavelength dependence of the dust emission as a function ofposition and environment across the disk of M33 at a linear resolution of 160pc using Spitzer and Herschel photometric data. Expressing the emissivity ofthe dust as a power law, the power-law exponent (beta) is estimated from twoindependent approaches designed to properly treat the degeneracy between betaand the dust temperature. Both beta and the dust temperature are higher in theinner disk than in the outer disk, contrary to reported beta-Tanti-correlations found in other sources. In the cold + warm dust model, thewarm component and the ionized gas (Halpha) have a very similar distributionacross the galaxy, demonstrating that the model separates the components in anappropriate fashion. The flocculent spiral arms and the dust lanes are evidentin the map of the cold component. Both cold and warm dust column densities arehigh in star forming regions and reach their maxima toward the giant starforming complexes NGC604 and NGC595. beta declines from close to 2 in thecenter to about 1.3 in the outer disk. beta is positively correlated with starformation and with molecular gas column, as traced by Halpha and CO emission.The lower dust emissivity index in the outer parts of M33 is likely related tothe reduced metallicity (different grain composition) and possibly differentsize distribution. It is not due to the decrease in stellar radiation field ortemperature in a simple way because the FIR-bright regions in the outer diskalso have a low beta. Like most spirals, M33 has a (decreasing) radial gradientin star formation and molecular-to-atomic gas ratio such that the regionsbright in Halpha or CO tend to trace the inner disk, making it difficult todistinguish between their effects on the dust.

Variation in the dust emissivity index across M33 with Herschel and Spitzer (HerM33es)