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/

Zendy Plus

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

Zendy Tools

Zendy Open

IC 2163 and NGC 2207 are interacting galaxies that have been well studied atoptical and radio wavelengths and simulated in numerical models to reproducethe observed kinematics and morphological features. Spitzer IRAC and MIPSobservations reported here show over 200 bright clumps from young starcomplexes. The brightest IR clump is a morphologically peculiar region of starformation in the western arm of NGC 2207. This clump, which dominates theHalpha and radio continuum emission from both galaxies, accounts for ~12% ofthe total 24mu m flux. Nearly half of the clumps are regularly spaced alongsome filamentary structure, whether in the starburst oval of IC 2163 or in thethin spiral arms of NGC 2207. This regularity appears to influence the clumpluminosity function, making it peaked at a value nearly a factor of 10 abovethe completeness limit, particularly in the starburst oval. This is unlike theoptical clusters inside the clumps, which have a luminosity function consistentwith the usual power law form. The giant IR clumps presumably formed bygravitational instabilities in the compressed gas of the oval and the spiralarms, whereas the individual clusters formed by more chaotic processes, such asturbulence compression, inside these larger-scale structures.Comment: 49 pages, 18 figures, ApJ, 642, 15

Spitzer Space TelescopeIRAC and MIPS Observations of the Interacting Galaxies IC 2163 and NGC 2207: Clumpy Emission